Scientific Committee on Solar-Terrestrial Physics (SCOSTEP)Scientific Committee on Solar-Terrestrial Physics (SCOSTEP)Scientific Committee on Solar-Terrestrial Physics (SCOSTEP)

International CAWSES SymposiumInternational CAWSES SymposiumKyoto, Japan; October 23–27, 2007Kyoto, Japan; October 23–27, 2007

ABSTRACTSABSTRACTS

Conveners T. Tsuda Research Institute for Sustainable Humanosphere, Kyoto University R. Fujii Solar-Terrestrial Environment Laboratory, Nagoya University K. Shibata Kwasan and Hida Observatories, Graduate School of Science, Kyoto

University

M. A. Geller Institute for Terrestrial and Planetary Atmospheres, the School of Marine and Atmospheric Sciences, Stony Brook University

Science Program Committee J. Alexander S. Avery D. Baker S. Basu J. Beer J.-L. Bougeret C. Z. Cheng J. Davis E. Friis-Christensen C. Frohlich K.-H. Glassmeier T. Gombosi N. Gopalswamy L. Gray M. Hagan J. Haigh L. Harra M. Hirahara T. Hirooka (co-chair) M. Hoshino T. Iyemori K. Kodera M. Kojima J. Kozyra K. Labitzke L. Lee C.-H. Liu M. Lockwood F.-J, Luebken T. Obara (co-chair) Y. Omura (chair) J. Pap A. Richmond J. Russell III T. Sakurai K. Sato (co-chair) B. Schmieder K. Shiokawa J. Sojka S. K. Solanki R. Vincent J. X. Wang S. T. Wu M. Yamamoto K. Yumoto L. Zelenyi Local Organizing Committee M. Akioka K. Fujiki T. Goka H. Kawano T. Kikuchi H. Kojima K. Kusano K. Maezawa T. Maruyama S. Masuda T. Murata R. Kitai T. Nakamura T. Ogino (chair) T. Ono A. Saito N. Sato Ki. Shibata S. Taguchi T. Terasawa F. Tohyama S. Tsuneta H. Usui S. Watanabe T. Watanabe T. Yokoyama

International CAWSES

Symposium

Kyoto, Japan October 23 – 27, 2007

Scientific Committee on Solar-Terrestrial Physics

Sponsored by

Scientific Committee on Solar-Terrestrial Physics (SCOSTEP)

Research Institute for Sustainable Humanosphere, Kyoto University Kwasan and Hida Observatories, Graduate School of Science, Kyoto University

Solar-Terrestrial Environment Laboratory, Nagoya University

Kyoto University Grant-in-Aid for Creative Scientific Research Project Basic Study of Space Weather Prediction

Kyoto University 21st Century COE Program Center for Diversity and Universality in Physics

Kyoto University 21st Century COE Program Elucidation of Active Geosphere

Nagoya University 21st Century COE Program Dynamics of Sun-Earth-Life Interactive System

National Institute of Information and Communications Technology (NICT)

In Cooperation with

Science Council of Japan

Astronomical Society of Japan Meteorological Society of Japan

Society of Geomagnetism and Earth, Planetary and Space Sciences Japan Geoscience Union

Supported by

Japan Society for the Promotion of Science

The Commemorative Organization for the Japan World Exposition ('70)

Message from the President of the Scientific Committee

on Solar Terrestrial Physics

Robert A. Vincent

It is a great pleasure to welcome participants to the CAWSES International Symposium. This year marks the 50th anniversary of the IGY, out which grew SCOSTEP and its research programmes, of which CAWSES is the just the latest. Planned to provide a comprehensive Sun-to-Earth view of the solar-terrestrial environment, CAWSES concludes in 2008. This meeting therefore provides an opportunity to survey the scientific outcomes and developments in our understanding that have come out of this program as well as an opportunity to consider whether the original goals are being met. The meeting is also an occasion to help plan future international SCOSTEP activities. Planning for CAWES-II is now well underway and the symposium is an occasion for participants to provide input into shaping the future of SCOSTEP. CAWSES has benefited greatly by the strong growth in scientific infrastructure in the past decade. New instruments installed in polar regions and on the equator provide a more comprehensive view of the atmosphere and ionosphere. New satellite missions enhance our view of solar phenomena and their impact on the Earth’s environment, while other missions now provide unprecedented views of the lower and middle atmosphere. We have also benefited from new ways to communicate. A significant innovation was the successful First Virtual Conference in Space Science in November 2006 in which scientists from all around the world participated over several days. There is no doubt that this activity brought our community closer together and it provides a template for future initiatives. Another innovation is the production as part of the CAWSES Capacity Building effort of the “Comic Books” by our Japanese colleagues at Nagoya University. Six comic books have been translated into English and are now being translated into other languages. I know from personal experience how much these books have stimulated the interest of schoolteachers and their students in solar-terrestrial phenomena. Initiatives such as this provide great opportunities to reach out to a new audience and to stimulate an interest in science in general and the field of solar-terrestrial relations in particular. This contribution to capacity building is another fine example of the fine contribution of Japanese scientists to SCOSTEP. The symposium provides another chance to acknowledge the generous support provided by the government, academic community and scientists of Japan to all of SCOSTEP’s activities.

Preface from the Conveners

SCOSTEP (Scientific Committee on Solar-Terrestrial Physics) began implementing its CAWSES (Climate and Weather of the Sun-Earth System) program in 2004, with it being scheduled to formally end at the end 2008. It seems appropriate as we near the end of CAWSES’ initial period of implementation to examine the progress that we have made as well as to look forward to the future. Thus, this international symposium on CAWSES is being held at Kyoto University, Kyoto, Japan during October 23-27, 2007. This meeting comprehensively covers the four major themes of CAWSES: 1) Solar Influence on Climate, 2) Space Weather, Science and Applications, 3) Atmospheric Coupling Processes, and 4) Space Climatology. The symposium will commence with an overview talk on CAWSES by Prof. S. K. Avery, the CASWES Coordinator. Three tutorial lectures by Prof. E. Parker, Prof. A. Nishida and Prof. M. A. Geller on the Sun, magnetosphere, and middle atmosphere will be given with the intent of introducing all participants to the various aspects of solar-terrestrial physics no matter what their specialty area. In the morning sessions, 16 keynote papers will be included. Again, the intent is to familiarize all participants to research on various aspects of the solar-terrestrial system. More specific research presentation sessions in the afternoon consist of 45 invited papers, 97 contributed talks and 222 poster papers. A total of 453 papers have been submitted to this symposium. These afternoon programs are organized by an international program committee, chaired by Prof. Y. Omura. The five full days of the symposium are composed of two parallel oral sessions and a poster session. In particular, we will hold a special session on space weather in recognition of Prof. Kamide's outstanding achievements in that and closely related fields. In addition to the plenary scientific sessions, smaller group discussions will also be organized in order to discuss future directions after the initial CAWSES period. A diverse group of experimentalists, modelers, and theoreticians with a variety of specialty areas, but who have a common focus on CAWSES, are participating in the meeting. We expect that a total of more than 400 scientists and students from 20 countries will participate in the symposium, with about 200 scientists coming from outside Japan. Since treating the entire solar-terrestrial domain as one system rather than treating each region independently is the central concept of CAWSES, we hope this meeting will provide a forum for all of the STP (Solar-Terrestrial Physics) scientists to review and discuss present and future directions of CAWSES research worldwide activities. We hope that all attending will find their symposium experience an enriching one and will continue contributing to CAWSES and to future SCOSTEP activities. We are deeply grateful to the local organizing committee lead by Prof. T. Ogino, who has contributed to the arrangements of this symposium devotedly.

Conveners: Toshitaka Tsuda Ryoichi Fujii

Kazunari Shibata

Marvin A. Geller

Scientific Committee on Solar-Terrestrial Physics (SCOSTEP)

BUREAU

President: R. A. Vincent (Australia) Vice President: B. Schmieder (France)

Scientific Secretary: Gang Lu (USA)

W. Baumjohann, Austria (IAGA) N. Gopalswamy, USA (IAU) M. Candidi, Italy (SCAR) K. Hamilton, USA (IAMAS) S. Chapman, U.K. (IUPAP) C. Hanuise, France (URSI) R. Fujii, Japan (COSPAR)

Climate And Weather of the Sun-Earth System (CAWSES) 2004-2008

TEAM

Chair: Susan Avery Scientific Coordinator: D. Pallamraju Program Administrator: Julia Barsky

SCIENCE STEERING GROUP

J.-L. Bougeret, FR J. Haigh, UK Y. Kamide, JP C.-H. Liu, TW A. Richmond, US L. Zelenyi, RU

Theme 1: Solar Influence on Climate

M. Lockwood - Co-Chair, UK L. Gray - Co-Chair, UK

Theme 2: Space Weather: Science and Applications J. Kozyra - Co-Chair, US K. Shibata - Co-Chair, JP

Theme 3: Atmospheric Coupling Processes:

F-J. Luebken - Co-Chair, DE J. Alexander - Co-Chair, US

Theme 4: Space Climatology: C. Fröhlich - Co-Chair, CH J. Sojka - Co-Chair, US

Table of Contents Tutorials - - --- ------ ---- ------ -------- ------ -------- ------ -------- ------ -------- ------ ----- 1

Keynotes - - --- ------ ---- ------ -------- ------ -------- ------ -------- ------ -------- ------ ---- 3

Oral Sessions SA11 Solar and Space Var iabi l i ty - - ------------------ -------------------- --------- 13

SA12 Short- term Solar Inf luence on Earth 's Environment --- ------ -------- -- 18

SA21 Solar Cycle and Long-term Response I - ----- ------ -------- ------ -------- - 23

SA22 Solar Cycle and Long-term Response I I - ---- ------ -------- ------ -------- - 28

SA31 Ionosphere - ------ ------ ------ -------- ------ -------- ------ -------- ------ -------- 32

SA32 Mesosphere and Thermosphere ----- ------ ---- ------ -------- ------ -------- - 36

SA41 Mesosphere and Lower Thermosphere------- ---- ------ -------- ------ -------- 39

SA42 Gravi ty Waves, Lagrangian Mot ions -- ------- ------ -------- ------ -------- -- 43

SA51 Dynamical Coupl ing , Equator ial Waves ----- ------ -------- ------ -------- - 47

SA52 Cl imate Dynamics, Radar and Opt ical Observat ions ----- ------ -------- 50

SB11 Observat ions of Solar-Terrestr ia l Environment I - - -- ----- ------ --------- 53

SB12 Observat ions of Solar-Terrestr ia l Environment I I - - - ----- ------ --------- 58

SB21 Solar Wind I - ------ ----- ------ -------- ------ -------- ------ -------- ------ ------- 62

SB22 Solar Wind I I - - ----- ----- ------ -------- ------ -------- ------ -------- ------ ------- 67

SB31 High Energy Part ic les - ------ ------ ------ -------- ------ -------- ------ -------- - 71

SB32 Special Session Comemorat ing Prof. Kamide's Achievements --- ---- 74

SB41 Magnet ic Reconnect ion and Part ic le Accelerat ion -- ----- ------ -------- - 77

SB42 Space Weather Model ing and Simulat ion ----- ------ -------- ------ -------- 82

SB51 Ground-based Observat ion -- ----- ------ -------- ------ -------- ------ -------- 87

SB52 Geomagnet ic Storms and Solar Cycle Var iat ion -- ----- ------ -------- 90

Poster Sessions P1 --- ------ -------- ------ -------- ------ -------- ------ -------- ------ -------- ------ ------- 93

P3 --- ------ -------- ------ -------- ------ -------- ------ -------- ------ -------- ------ ------- 154

Author Index - - -- ------ ------ -------- ------ -------- ------ -------- ------ -------- ------ ---- 213

T1

Hydrodynamics, Magnetohydrodynamics, and Electric Circuit AnalogsEugene N. Parker

Department of Physics, University of Chicago, Chicago, IL 60637, USA

The large-scale bulk dynamics of a magnetized plasma is generally treated within the concepts of hydrodynamics(HD) and magnetohydrodynamics (MHD). Yet questions are sometimes raised about the applicability of HD andMHD and suggesting that electric currents are a better representation, from which there has grown a popular beliefin an electric circuit analog for the dynamics.We begin by showing in a collisionless gas how HD follows directly (using Gauss's theorem) from conservationof particles, momentum, and energy, given only that there are enough particles that the local mean particle densityis statistically well defined. Then, if there are enough free electrons and ions in the gas to neutralize any significant electric field in the movinglocal reference frame of the gas, MHD is an immediate consequence. The magnetic field is transported bodilywith the gas, and electric fields play no dynamic role.The effects (Hall current, Pedersen resistivity, Ohmic dissipation) arising in a partially ionized gas are small-scale,becoming negligible under most circumstances in any large-scale setting, but important in the local structure ofshock fronts and rapid reconnection, of course.Finally, it is shown that the inductive effects in the conventional current analog do not apply to the currentsflowing in a swirling magnetized plasma, because the plasma moves in the frame of reference in which there is nosignificant electric field

T2

Early Japanese Contributions to Space Weather ResearchAtsuhiro Nishida

Graduate University for Advanced Studies, Hayama, Kanagawa, Japan

Over a time period of two decades between the end of the WWII and early 1960s, the foundation of the SpaceWeather Research was built upon remote-sensing observations of the ionosphere, magnetosphere, heliosphere andthe sun that were conducted from the ground. We review pioneering works by Japanese scientists that contributedsignificantly to advances made during this epoch. Ingenuity and insight of our predecessors who could extractkey information from limited information are truly impressive. These early works benefited also from the heritageof earlier times, the community efforts to promote interactions, and the gradual development of the internationalcooperation. A happy marriage between basic science and application can be seen in some notable cases.

- 1 -

T3

1960s Advances in Middle Atmosphere ResearchMarvin A. Geller

Stony Brook University, Stony Brook, NY, USA 11794-5000

The 1960s might be referred to as the "Golden Age for Atmospheric Waves," and advances made during thatdecade have set the stage for many areas of research into Atmospheric Coupling Processes. Important papers inthis general area include Hines' classic paper on gravity waves; Matsuno's classic paper on quasi-geostrophicmotions near the Equator; Kato and Lindzen's independent discovery of missing Hough function modes; theindependent discovery of the quasi-biennial oscillation by Reed and by Ebdon and its subsequent successfultheoretical explanation by Lindzen and Holton; the Charney-Drazin theory for vertical planetary wave propagation(with important later contributions by Dickinson and Matsuno); the non-interaction concepts by Eliassen and Palmand by Charney and Drazin; the need for wave drag to explain the mesospheric circulation by Leovy; gravitywave critical level theory by Booker and Bretherton; and surely others that I haven't mentioned. Many other important research topics also had important beginnings in the 1960s. For instance, it was in 1965that the HOx catalytic cycle for destruction of stratospheric ozone was first suggested. Lively discussionsoccurred as to whether measurements of a very dry stratosphere were real or not. Pioneering rocket experimentstook place during the 1960s on mesosphere structure and its relation to noctilucent clouds. Early clear air echoeswere noted during the 1960s that helped to lay the foundation for MST radars, now an important mainstay ofmiddle atmosphere research. These latter two research areas helped to establish the basis for today's research intoPMSEs. Early transport-chemistry models of the middle atmosphere were appearing, as were the first generalcirculation models of the troposphere/stratosphere. These works have evolved into present-daytroposphere-middle atmosphere chemistry-climate models. A few examples are given to trace some of today's research areas back to their early, foundational phases duringthis pivotal decade for middle atmosphere, the 1960s.

- 2 -

K1-1

Evidence for Solar Forcing: Some Selected AspectsJuerg Beer

EAWAG, CH-8600 Duebendorf, Switzerland

Satellite based measurements over the past 30 years reveal typical changes in the total solar irradiance (TSI) of0.1% during an 11-y Schwabe cycle. The corresponding changes in the UV part of the spectrum are much largerbut do not contribute much to the TSI. Other potential forcing mechanisms related to the Sun are negligible as faras the involved power is concerned. It is not clear yet whether larger changes occur on longer time scales and towhat extent the forcing signal is amplified within the non-linear climate system.Therefore, detection and attribution of solar forcing is a difficult task. A promising approach is to compare recordsof solar activity with reconstructed climate changes based on palaeodata. Although it is still impossible to quantifythe solar forcing in W/m2 qualitative changes and periods of extreme solar activity such as grand minima can bederived from cosmogenic radionuclides (10Be, 14C). Using specific features of the reconstructed solar activity inthe time and frequency domain it is possible to provide strong evidence for solar forcing during earlier times whenthe content of greenhouse gases in the atmosphere was much smaller than today and rather constant.

K1-2

Winter Variability in the Stratosphere: Coupling between the Artic and theTropicsKarin Labitzke

Institute for Meteorology, Free University Berlin, Germany

Large effects of solar variability related to the 11-year sunspot cycle (SSC) are seen in the stratosphere, especiallyover the Arctic, but only if the data are grouped according to the phase of the QBO. New results based on anextended, 66-year long data set fully confirm earlier findings and suggest a significant effect of the SSC on theoccurrence of the Major Midwinter Warmings (MMWs) as well as on the strength of the stratospheric polar vortexand on the mean meridional circulation.By means of teleconnections the dynamical interaction between the Arctic and the Tropics in the stratosphere andin the troposphere is shown for the whole data set and compared with the anomalies of single events.The results suggest strongly that during the northern winter the teleconnections between the Arctic and theTropics were determined by the MMWs and the COLD winters, respectively. These events in the stratospheredepend, however, on the 11-year SSC and on the QBO.

- 3 -

K1-3

Hinode "A New Solar Observatory in Space"Saku Tsuneta

National Astronomical Observatory of Japan, Japan

Since its launch in September 2006, Japan-US-UK solar physics satellite, the Hinode, has continued itsobservation of the sun, sending back solar images of unprecedented clarity every day. The Hinode is equippedwith three telescopes, visible light telescope, X-ray telescope, and extreme ultraviolet imaging spectrometer. Theoptical telescope has a large primary mirror measuring 50 centimeters in diameter, and is the world's largest spacetelescope for observing the sun and its vector magnetic fields. The impact of the Hinode optical telescope on solarphysics is comparable to that of the Hubble Space Telescope on optical astronomy. While the optical telescopeobserves the sun's surface, the X-ray telescope captures images of the corona and the high-temperature flares thatrange between several million and several tens of millions of degrees. The telescope has captured coronalstructures that are clearer than ever. The EUV imaging spectrometer possesses about ten times the sensitivity andfour times the resolution of a similar instrument that is provided on the SOHO satellite.The source of energy for the sun is in the nuclear fusion reaction that takes place at its core. The temperaturedrops closer to the surface, where the temperature measures about 6,000 degrees. Mysteriously, the temperaturestarts rising again above the surface and the temperature of the corona is exceptionally high at several millions ofdegrees. It is as if water were boiling fiercely in a kettle placed on a fireless stove, inconceivable as it may sound.The phenomenon is referred to as the coronal heating problem, and it is one of the major astronomical mysteries.The Hinode observatory was designed to attack the problem. We expect that there would also be clues tounraveling why strong magnetic fields are formed and how solar flares are triggered. Overview on the initial results from Hinode is presented. Dynamic video pictures captured by the Hinode can beviewed on the website of the National Astronomical Observatory of Japan (NAOJ),http://hinode.nao.ac.jp/index_e.shtml.

K2-1

Mechanisms for Solar Influence of Earth's ClimateJoanna D. Haigh

Space and Atmospheric Physics, Blackett Laboratory, Imperial College London, London SW7 2AZ, UK

There is increasing evidence that changing solar activity over the 11-year solar cycle influences the Earth's climatealthough details of the mechanisms involved remain uncertain. One of the main problems is that the observedresponse appears to be too large to be explained entirely by the direct impact of changes in total solar irradianceon the surface and lower atmosphere. The temperature changes observed in the troposphere over the solar cycle are non-uniform and these areaccompanied by variations in tropospheric circulation. A weakening and poleward shift of the mid-latitude jets,along with a weakening and expansion of the tropical Hadley cells and a poleward shift of the Ferrell cells, isfound at solar maximum relative to solar minimum. These circulation changes, along with the non-uniformtemperature changes, point towards a dynamical response rather than simply altered direct radiative forcing. Climate modelling studies have demonstrated that similar tropospheric circulation and temperature changes tothose seen over the solar cycle can be produced by a dynamical response to increased heating of the stratosphere. The model results also suggest that the response of stratospheric ozone to solar variability may be importantbecause it plays a part in determining the stratospheric temperature signal. Thus a possible explanation for thetropospheric temperature and circulation changes may be found through a dynamical response to UV absorption inthe stratosphere.In this talk I will first briefly review the evidence for a solar cycle influence on the troposphere and consider theimpact of variations in solar UV on stratospheric temperature and composition. I will then assess to what extentgeneral circulation models are able to reproduce the apparent tropospheric solar signals. Finally I will presentsome recent work designed to investigate how altered stratospheric heating could produce such a response in thetroposphere: specifically the mechanisms involved in stratosphere-troposphere dynamical coupling.

- 4 -

In these studies we have used a simplified general circulation model and carried out spin-up ensembleexperiments to study the development of the response to an applied stratospheric heating perturbation. Resultssuggest that changes in the propagation of synoptic scale waves are important in transmitting the effect of alteredstratospheric heating to the troposphere below. This is further emphasized by the much weaker troposphericresponse found in a zonally symmetric experiment in which the stratospheric temperature was altered but the eddyfluxes remain fixed.

K2-2

Coronal Mass Ejections and Space WeatherNat Gopalswamy

Solar System Exploration, Code 695 NASA Goddard Space Flight Center Greenbelt, MD 20771, USA

Coronal mass ejections (CMEs) have been found to be the most energetic phenomenon in the heliosphere, thanksto the continuous and uniform data set obtained by the ESA/NASA Solar and Heliospheric Observatory (SOHO)mission. CMEs contribute to two major Space Weather elements: geomagnetic storms and high energy particles. Even though more than 11,000 CMEs have been observed by SOHO, only about 10% of them make a significantimpact on the heliosphere. This talk will consider this subset of CMEs, which are highly relevant for SpaceWeather, one of the key aspects of the CAWSES program. Halo CMEs, fast and wide CMEs, shock-drivingCMEs, and CMEs resulting in interplanetary ejecta all have the common property of being very energetic. Theireruptive location on the Sun leads to different types of impact on geospace. For example, fast and wide CMEsoriginating on the western hemisphere of the Sun are most important for producing particle radiation hazard ingeospace. On the other hand, geoeffective CMEs (the ones causing geomagnetic storms) need to be ejected rightclose to the solar disk center for direct impact on Earth. Shock-driving CMEs are easily identified usinglow-frequency radio emission detected by spaceborne experiments such as on board the Wind spacecraft. Afterviewing the properties of these special populations of CMEs, I will discuss future efforts needed to fullyunderstand these CMEs from the point of view of Space-Weather consequences.

- 5 -

K2-3

CAWSES Activities in Germany with Special Emphasis on Mesospheric IceLayersFranz-Josef Luebken

Leibniz Institute of Atmospheric Physics, Kuehlungsborn, Germany

The German Science Foundation (Deutsche Forschungsgemeinschaft, DFG) has initiated a priority programme forCAWSES for a period of 6 years. The second phase covers the years 2007-2009. More than 25 institutions and 80scientists within Germany are involved. In this presentation some highlights from the first period will be presentedregarding the following topics: characteristics of solar radiation and its influence on trace gases and aerosols fromthe stratosphere to the lower thermosphere, dynamical coupling mechanisms by waves and turbulence,microphysical processes in cloud generation, and long term changes of composition, temperatures, and winds.Special emphasis will be put on ice layers at the summer mesopause known as noctilucent clouds (NLC), polarmesosphere summer echoes (PSME), and polar mesospheric clouds (PMC). Observations from ground based andsatellite borne instruments(e.g. lidar, radar, spectrometers etc.) will be summarized and be compared with modelsimulations of the morphology of ice layers. Interhemispheric similarities and differences of cloud properties areexplained with a new model called LIMA (Leibniz Institute Model of the Atmosphere).

K3-1

Storm-Substorm RelationshipsY. Kamide

RISH, Kyoto University, Japan

Most of the Dst variance during intense geomagnetic storms can be reproduced reasonably well by changes inlarge-scale electric fields in the solar wind alone, but satellite observations of the ring current constituents duringthe main phase of magnetic storms show the importance of ionospheric ions, implying that ionospheric ionsassociated with the frequent occurrence of intense substorms are accelerated upward along magnetic field lines,contributing to the energy density of the storm-time ring current. An apparent controversy thus exists regardingthe relative importance of the two processes. This paper contends that, during magnetic storms, the quasi-steadycomponent of the interplanetary electric fields is important in enhancing the storm-time ring current, while thevariability in the solar wind electric fields are responsible for initiating substorms. As in a "thought" experiment, ifone were to control the solar wind, i.e., to generate purely steady southward interplanetary magnetic field, theresult would be a geomagnetic storm during which no substorm expansions take place.

- 6 -

K3-2

New Discoveries from CAWSES International Space Weather CampaignsJanet U. Kozyra

University of Michigan, 1414 Space Research Bldg, 2455 Hayward, Ann Arbor, MI 48109-2143, USA

The sun, heliosphere, magnetosphere, ionosphere and atmosphere together form a complex system of systems,which is in general out-of-equilibrium and evolutionary in nature. In a very real sense, these Sun-Earth systemcharacteristics dictate the research strategies needed to accelerate progress. To explore such a system,observations from a single-spacecraft are no longer enough; multi-spacecraft observations covering both micro-and macro-scales at strategic locations from Sun-to-Earth are essential. Ground-based instruments and networksof sensors when joined provide global views of quantities that are impractical or impossible to obtain fromspacecraft. And telescopes distributed around the globe provide continuous observations of the Sun. Thecoordination of these data sets is an international effort. Grand challenge science questions are interdisciplinary innature spanning multiple regions or, at times, the entire system sun-to-Earth. A number of CAWSES campaignsand data analysis workshops were undertaken to draw together comprehensive international data sets describingthe state of the Sun-Earth system during space weather disturbances, focus attention on open science questions,and facilitate interdisciplinary interactions among scientists, and students worldwide. The aim of this talk is topresent some of the exciting scientific discoveries that resulted from these global interactions.

K3-3

Simulating and Predicting Solar 'Climate'Mausumi Dikpati

High Altitude Observatory, National Center for Atmospheric Research, 3080 Center Green, Boulder, CO 80301, USA

Understanding and predicting the solar activity cycle remains one of the key problems within solar physics.Predictions are needed ever more as government and commercial industries continue to expand into space andemploy technologies on the ground that are sensitive to solar activity. With the progress of observational andtheoretical knowledge, the global-scale solar dynamo models have reached the stage that it is possible to calibratethem for the Sun by adjusting only a few tunable parameters. The important ingredients in a dynamo model that ismost plausibly calibrated are differential rotation (Omega-effect), helical turbulence (alpha-effect), meridionalcirculation and turbulent diffusion. The meridional circulation works as a conveyor belt for transporting themagnetic flux and governs the dynamo cycle period. Meridional circulation and magnetic diffusivity togethergovern the memory of the Sun's past magnetic fields. After describing the physical processes involved in this classof dynamo, we will show that a predictive tool can be built from it to predict the solar 'climate', namely the meansolar cycle features, particularly cycle amplitude and duration, by assimilating magnetic field data from previouscycles. We will discuss the successes, limitations and future prospects for such predictive solar dynamo models.

- 7 -

K3-4

Coupling Processes in the Equatorial Atmosphere (CPEA)Shoichiro Fukao

1. Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Kyoto 611-0011, Japan2. Research Institute of Science and Technology, Tokai University, 2-28-4 Tomigaya, Shibuya, Tokyo 151-0063, Japan

The Indonesian Archipelago is one of the centers of intense atmospheric motions over the globe. The mechanismsof these atmospheric motions and their changes, however, have not yet been made clear due to the sparseness ofobservational data in that region. The Coupling Processes in the Equatorial Atmosphere (CPEA), a six-yearresearch project of Japan, was conducted in Indonesia to observationally elucidate dynamical andelectrodynamical coupling processes occurring in the equatorial atmosphere from September 2001 to March 2007.

During six years of CPEA, a new Equatorial Atmosphere Observatory was established with the EquatorialAtmosphere Radar (EAR) as the core facility in Kototabang, West Sumatra, Indonesia (0.20??S, 100.32??E). Inthe present talk we will review some highlights from this project. First, it has been found, contrary to the traditional expectation, that deep convection over Sumatra Island isobserved in inactive phase of Madden-Julian Oscillation (MJO), while shallow convection is dominant in activephase. Secondly, clear correlation between deep convection and enhanced inertia gravity waves with period 2-3days was found with their wave source identified as slowly eastward advecting convection. Thirdly, Kelvin waveswith periods 10-12 days near the tropopause and 5.5-8 days in the lower stratosphere were detected locally overIndonesia and globally by CHAMP-GPS. Fourthly, several pieces of evidence have been provided to demonstratethat long-term variability in the troposphere influences the dynamics of the mesopause-homopause region. Finally, it has been suggested that gravity waves near 100 km in altitude contribute to generation of plasmabubbles.

K4-1

Magnetic Reconnection in the Solar Wind: An OverviewJohn T. Gosling

Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA

Quasi-stationary magnetic reconnection occurs frequently at thin current sheets in the solar wind over a largerange of heliocentric distances. Evidence for reconnection is found in observations of Petschek-type exhausts, i.e.,exhausts of jetting plasma bounded by back-to-back rotational discontinuities. The exhausts are identified asroughly Alfvenic accelerated plasma confined to field reversal regions that almost always take the form ofbifurcated (double-step) current sheets. They are embedded within the solar wind flow and are convected past aspacecraft on time scales ranging from seconds up to several hours, with time scales less than 100 s being mostcommon. The exhausts are observed predominantly in the low-speed solar wind or in association withinterplanetary coronal mass ejections in plasma predominantly having low proton beta. Near solar minimumreconnection exhausts are swept past Earth at a rate of about 1.5 events/day. Reconnection in the solar windoccurs most frequently at magnetic field shears < 90 degrees; exhausts associated with local field shears as low as24 degrees have been identified. Multi-spacecraft observations provide convincing evidence that the exhaustscommonly result from prolonged reconnection at extended and continuous X-lines. A relatively minor fraction ofreconnection exhausts are found at the heliospheric current sheet, HCS, but observations at the HCS areparticularly useful for demonstrating particle interpenetration within the exhausts and magnetic field topologychanges associated with reconnection. Although reconnection exhausts are characterized by bulk plasmaacceleration, we have not yet found evidence for additional particle acceleration in these events.

- 8 -

K4-2

Maqnetotail after GEOTAIL, INTERBALL and CLUSTER: AcceleratedBeams, Thin Current Sheets and Intermittent TurbulenceLev M.Zelenyi

Space Research Institute, Profsoiuznaia ,84/32, Moscow 117997, Russia

Magnetic tail of the Earth is produced in the course of interaction of supersonic stream of solar wind plasma withthe rather strong (on a cosmic scales) magnetic field of our planet. Energy which drives the magnetosphericdynamics is coming from the solar wind and could be temporarily stored in the magnetotail. Magnetotail plays the principal role in the large scale energy circulation in the Sun-Earth system due to its metastable properties. Last 15 years brought completely new understanding of both global (MHD scales) and local (kinetic scales)characteristics of this region. Starting from ISTP program and multisatellite IACG campaigns researches gainmuch deeper understanding of both the magnetotail topology and its driven (and intrinsic) dynamics.Geotail, Interball, Wind and Polar coordinated measurements gave the momentum to the global MHDmodeling of magnetospheric dynamics driven by the upstream solar wind parameters. However, the multiscale character of magnetotail plasma processes required to make the next step and study the sub MHD physics at smaller (~ ion Larmor radius) scales. Earlier ISEE 1, 2 measurements gave a few indications on theimportance of the corresponding small scale effects . These investigations were continued by the dualmeasurements of Interball-1, Magion-4 pair, which explored the peculiarities of the high latitude tailmagnetopause. The major breakthrough was made during the last few years after the launch of Cluster. At the periods of smallest separations between Cluster s/c the measurements at the upper edge of kinetic scales revealed the existence ofcomplicated 3 dimensional thin plasma structures both at the center of plasma sheet and its edges near the magnetic separatrix between open and closed field lines. So called thin current sheets found near the tail midplane demonstrated multilayered and often asymmetric structure, often subjected to a strong kink-like distortions. The echoes of a powerful acceleration processes operating in the distant regions of magnetotail could be seen inthe high-latitude auroral region as VDIS (Velocity Dispersed Ion Structures) often fragmented at a sets of isolatedsub-structures. Dynamical plasma processes occurring in this region have very complicated spatial/temporalmanifestations. Thermal ions in the tail are as a rule non-adiabatic and are accelerated downstream in the tail byFermi-II type mechanism. Resonant interactions produce fragmentation of accelerated ion beams on a finitenumber of substructures.Due to the weakness of magnetic field in a field reversal region near the tail midplane even electrons couldbecome non-adiabatic and are non-capable to provide the rigidity to field lines which becomes stochastic. Suchsheets have more chances to be observed far downstream of the tail at the open field lines. Complex topology ofmagnetotail field in this region is self-consistently coupled to the distribution of plasma currents which particlesshould carry moving in such entangled magnetic geometry. Multiscale magnetic structures are mostly frozen tothe convecting magnetotail plasma. Complicated character of these interactions, influence of boundaries andvariability of solar wind driving often made the resulting turbulence intermittent.Important results are expected from the THEMIS mission launched this year and especially from the newambitious international perspective projects aimed at studies of the physics already at the electron scales (Scope,Cross Scale , Roi)Acknowledgments This work is partially supported by RFBR grants 07-02-00319, 06-02-72561, ScientificSchools grant HIII-5359.2006.2 and INTAS grant 06-1000017-8943

- 9 -

K4-3

Tidal Coupling from the Troposphere to the Thermosphere-IonosphereSystemJeffrey M. Forbes

Department of Aerospace Engineering Sciences, University of Colorado, Boulder, CO 80309, USA

In this talk I will provide a perspective on the global manifestations and consequences of the semidiurnal tide inEarth's atmosphere. Topics to be addressed include tide/mean-wind interactions; production ofnon-Sun-synchronous tides due to latent heating due to deep tropical convection, and by nonlinear interactionbetween sun-synchronous tides and stationary planetary waves; tidal modulation by planetary-wave oscillations atquasi-2-day and -10-day periods and related effects in the thermosphere-ionosphere system; modification of thezonal mean circulation due to momentum deposition by dissipating tides; and the lunar semidiurnal tide,especially new observations in the MLT region temperature field and in thermosphere densities near 400 km. Experimental and modeling evidence for all of the above phenomena will be presented, so as to provide anappreciation for the pervasiveness of semidiurnal tidal effects from the surface to the ionosphere-thermospheresystem.

K5-1

Gravity Wave Coupling in the Middle AtmosphereRobert A. Vincent

Physics, University of Adelaide, Adelaide 5005, Australia

Atmospheric gravity waves efficiently couple energy and momentum from source regions in the lower atmosphereto the middle atmosphere and ionosphere. The CAWSES period has seen significant advances in the study ofgravity waves and their effects. Observational advances come from the availability of new ground andspace-based instruments, together with in situ observations using long-duration superpressure balloons. Theresults provide important information on the spatial and temporal variability of wave activity and sources. Thistalk will review some of these advances and their implications for gravity wave coupling in the middle and upperatmosphere.

- 10 -

K5-2

Calibrating Sunspot Numbers Using the Magnetic NeedleLeif Svalgaard

ETK

Solar FUV creates and maintains the ionosphere. Thermal winds and solar tides drive a dynamo creating a currentsystem whose magnetic effect is readily observed on the ground. Observations of this diurnal magnetic signatureof the FUV flux (and indirectly, the sunspot number) go back more that 250 years and can be used to estimate thesunspot number in the past, fording an independent calibration of the sunspot number time series. We show thatboth the Zurich and the Group Sunspot Numbers are too small before cycle 18 with the discrepancy growinglarger as we go back in time, reaching more than 50%.

K5-3

Total Solar Irradiance : What Have We Learned about Its Variability fromthe Record of the Last Three Solar Cycles?Claus Fröhlich

Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, CH 7260 Davos Dorf, Switzerland

Since November 1978 a set of total solar irradiance (TSI) measurements from space is available, yielding a timeseries of almost 30 years. Presently, there are three TSI composites available, called PMOD, ACRIM and IRMB,which are all constructed from the same original data, but use different procedures to correct for sensitivitychanges. The PMOD composite is the only one which also corrects the early HF data for degradation. Thus, it canbe used to study TSI variability over the last three activity cycles with special emphasis on similarities anddifferences. A still open question is whether a long-term trend of TSI can be identified from the present measured TSI. This isobviously related to the ability to correct for the degradation of the idividual radiometers used to measure TSI.Together with a comparison to a 3-component proxy model and other indices of solar activity the use of this timeseries as a basis for the reconstruction of TSI into the past will be discussed.

- 11 -

- 12 -

SA11I-1

Diagnostics of Solar Subsurface Weather by HelioseismologyAlexander Kosovichev

Stanford University, USA

Helioseismology observations of the Sun's interior have revealed large-scale flow patterns, associated withdeveloping solar activity. These flows determine the "solar subsurface weather". Their investigation is critical forour understanding of the mechanisms of solar activity. I'll present recent results of investigation of emergence ofmagnetic flux, formation of active region and subsurface dynamics of flaring activity. Also, I'll discuss attempts todevelop predicting capabilities based on helioseismology measurements, and plans for the Solar DynamicsObservatory mission.

SA11I-2

CME 3D Reconstructions Using Solar Mass Ejection Imager andInterplanetary Scintillation Data and Extrapolation to UlyssesBernard V. Jackson1, P. Paul Hick1, Andrew Buffington1, Mario M. Bisi1, Elizabeth A. Jensen1, Masayoshi Kojima2, and Munetoshi Tokumaru2

1. CASS-UCSD, 9500 Gilman Drive, La Jolla, CA 92093-0424, U.S.A.2. STELab, Nagoya University, Furo-cho Chikusa-ku, Nagoya, Aichi, 464-8601, Japan

We have available a UCSD 3D reconstruction technique that obtains perspective views from solar corotatingplasma and outward-flowing solar wind as observed from Earth by iteratively fitting a kinematic solar wind modelto either Solar Mass Ejection Imager (SMEI) or interplanetary scintillation (IPS) observations or a combination ofthese two data sets. This 3D modeling technique permits reconstruction of the density and velocity of corotatingstructures and CMEs. In this ongoing study, we compare SMEI and STELab observations (both direct and usingthe 3D reconstructions) from data obtained this year while the Ulysses spacecraft is near the Sun and the STEREOspacecraft are near Earth, and extrapolate these observations to the Ulysses spacecraft. Our observations provideremote-sensing measurements and global context for heliospheric structures which here-to-fore have beeninterpolated between and extended from multi-spacecraft observations. We do this as well to determine noise fromsignal in the data sets, to discover the differences between the SMEI and IPS remote-sensing data sets, and tocertify the UCSD 3D reconstruction technique by comparison with solar wind in-situ observations from spacecraftdistant from Earth.

- 13 -

SA11I-3

Solar Irradiance Variations: from Days to MilleniaY. C. Unruh and S. K. Solanki

Max-Planck-Institut fuer Sonnensystemforschung

The solar magnetic field is strongly variable on many different time scales.This variability is reflected by the variability of solar activity and irradiance. Direct measurements of total solarirradiance are avilable only since 1978, those of spectral solar irradiance for an even shorter period of time.Therefore, longer records of solar irradiance, as are required for global climate change studies, need to bereconstructed using models. A hierarchy of models is being constructed that covers an increasingly longer periodof time. For the period since 1974 it is possible to reproduce the measured total and spectral irradiance with highaccuracy using measurements of surface magnetic fields, while for the period since the Maunder minimumsunspot number data are used to guide the reconstruction. On longer time scales cycle-averaged sunspot numbersare employed. A full set of such models has now been constructed for total solar irradiance. The modeling ofspectral irradiance is currently underway.

SA11-1

Flare-CME Geometry in the Longitudinal DirectionS. Yashiro1, N. Gopalswamy2, G. Michalek1, H. Xie1, S. Akiyama1, and R. A. Howard3

1. Catholic University of America, Washington, DC 20064, USA2. NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA3. Naval Research Laboratory, Washington, DC 20375, USA

Yashiro et al. (2007) examined the flare positions with respect to the CME span and found that most frequent flaresite is the center of the CME span. However, since the spatial relationship was investigated by analyzing the limbevents, the finding can apply only in the latitudinal direction. In this paper we examine flare-CME geometry in thelongitudinal direction by analyzing the shape of halo CMEs associated with flares occurring at the middle of thesolar disk (CMD =< 5 degree). If the flares were located at one end of the longitudinal span of the CMEs, theCME should appear with the asymmetric shape in the east-west direction. During 1996 - 2006 (inclusive), therewere 33 flare-CME events which satisfied the above criteria. Out of the 33 events, 13 halos did not havesignificant asymmetry, 13 halos had asymmetry in the north-south direction, and 7 halos had asymmetry in theeast-west direction. The north-south asymmetry of the halos was depended on whether the events occurred in thenorth or in the south hemisphere. This result suggests that the some flares are located at the longitudinal end of theCME span, but the majority is located at the center of the CME span. By applying a cone model to the 33 halos,we discuss the flare-CME geometry in detail.

- 14 -

SA11-2

A Forecasting Study of the Dynamic Heliosphere Using Solar and SolarWind ObservationsHaruichi Washimi1, Gary, P. Zank1, Qiang, Hu1, and Takashi Tanaka2

1. Institute of Geophysics and Planetary Physics (IGPP), University of california, Riverside, CA 92521, USA2. Faculty of Science, Kyushu University, Hakodate, Fukuoka 812-8581, Japan

We present results that describe the 'climate and weather of the sun-heliosphere system (CAWSHS)' on the verylargest heliospheric scales. Voyager 1 (V1) crossed the termination shock (TS), located at 94 AU from the sun, inlate 2004. Voyager 2 (V2) is approaching the TS in the southern hemisphere, and the combined Voyagerobservations now make the study of the temporal heliospheric structure possible, albeit a challenging problem. Wehave found using highly resolved MHD simulations that a pressure-pulse is driven into the heliosheath byvariations in the interplanetary ram-pressure of the supersonic solar-wind. In the heliosheath, the pulse propagatesfrom the TS to the heliopause (HP), where it is partially reflected at the HP (and partially transmitted), whereuponit then propagates back to the TS, thereby slowing the outward motion of the TS and hence changing the TSlocation. Thus, in addition to directly responding to upstream supersonic solar wind disturbances, the TS locationis found to change in response to incident downstream disturbances associated with waves reflected from the HPproduced by earlier supersonic solar wind disturbances. Waves and disturbances in the heliosheath are thus foundto play an important role in the dynamic structure of the large-scale heliosphere. To determine the time-varyingTS position, we incorporate V2 plasma data as a boundary condition into our 3D MHD simulations, which allowsus to forecast the termination shock movement for nearly a year after the present V2 data.To carry out a more detailed analysis of the heliosphere and also to continue to identify the TS and HP locationsafter the expected V2 crossing TS in a few years, we need CAWSHS to provide direct derivations of reliablesolar-wind speeds and densities by using MHD simulations based on observations of photospheric and coronalconditions. Some specific examples will be shown.

SA11-3

A Systems Approach Toward Solar-Terrestrial Research as Facilitated byCAWSES CampaignsGang Lu

High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO, USA

Earth's ionosphere and upper atmosphere are subject to several geophysical forcings originating from the Sun. The interaction between the solar wind and the Earth's magnetosphere results in a fraction of the solar windenergy and plasma being transmitted into the magnetosphere, and subsequently into the ionosphere and upperatmosphere in the forms of auroral precipitation and Joule frictional heating. Solar energetic particles penetrateinto the upper and middle atmosphere to cause significant ionization and chemical effects. Solar UV and EUVradiations are the main energy source for heating, ionization, and photochemical reactions in the upper atmosphereand ionosphere. This paper discusses the progresses made in understanding the Sun-Earth connection throughcomprehensive observational and modeling effort during coordinated CAWSES campaigns. In particular,observational and numerical modeling results during the September 2005 CAWSES campaign event will beshown to illustrate the complex responses of the ionosphere and thermosphere to various solar andmagnetospheric forcing.

- 15 -

SA11-4

Radio-Optical Mechanism for the Solar and Magnetospheric Influence onthe Weather and ClimateSergey V. Avakyan and Nikolai A. Voronin

All-Russian Scientific Center

A new approach is suggested for the physical mechanism of the solar and geomagnetic activity influence on theweather and climate characteristics. The new approach is based on the experimental data and on already the testedschemes which involve condensation mechanism and take into account the influence of generated clusters on theatmosphere transparence at the altitudes higher than 3 km.Essentially new are the following two positions:1) Taking into account generation in the terrestrial ionosphere of the microwave radiation which intensity risesduring solar flares and geomagnetic storms. As a source of the microwave radiation we propose to consider theprocess of excitation of Rydberg states in atoms and molecules of the upper atmosphere gases by energeticionosperic electrons namely photoelectrons, secondary electrons and Auger electrons. This radiation in thewavelength range from 1 mm and longer nearly freely penetrates down to the atmosphere base and carriescomplete information on the intensity and time dependence of the ionizing electromagnetic flux from the Sun andalso of the magnetospheric corpuscular precipitations (energetic electrons and protons) to the ionosphere duringgeomagnetic storms.2) Taking into account Rydberg states excitation at the preliminary stages of association and dissociation ofclusters (as well as ion clusters) of water and carbon dioxide. The rates of association and dissociation processesdepend strongly on the magnitude of the Rydberg state orbital quantum number. An increase in the orbitalquantum number by one results in a decrease of cross-sections of the dissociation processes by an order ofmagnitude. According to the developed theory this increase in the quantum number is caused by stimulatedabsorption of the ionospheric microwave radiation quanta as well as solar radiobursts radiation quanta during theperiods of increased solar and geomagnetic activity.Thus we suggest three-stage radio-optical trigger mechanism for the influence of solar flares and geomagneticstorms on the weather characteristics. The first stage is an increase in generation of the microwave radiation whichpenetrates from the ionosphere to the earth surface. The second stage is a change in the proportion of water vapourto water clusters as well as proportion of carbon dioxide gas to carbon dioxide clusters caused by increasedmicrowave radiation. The third stage is a change of the atmosphere transparence in the absorption bands of watervapour and of carbon dioxide and also a rise and deepening of the absorption bands of clusters. The atmospheretransparence at the altitudes higher than 3 km determines the fluxes of solar irradiance coming down to thenear-earth altitudes as well as flux of the thermal radiation coming out from the underlying surface. These fluxesform the basis of the thermal balance and affect the weather characteristics of the lower atmosphere.The appropriation and next using of this three-stage mechanism of the Sun - weather links may be the task of theCAWSES Themes: 1 (Solar Influence on Climate), 2 (Space Weather), and 4 (Space Climatology), it is possible,in the frame of the International Science and Technology Center (Moscow) project.

- 16 -

SA11-5

CAWSES - India : An OverviewP. B. Rao, R. Sridharan, S. C. Chakravarty, and Kusuma G. Rao

1. National Remote Sensing Agency, Hyderabad 500 037, India2. Space Physics Laboratory, VSSC, Trivandrum 695 022, India3. ISRO Headquarters, Bangalore 560 094, India

The paper presents an overview of the CAWSES-India program, highlighting some new findings concerning theequatorial and low latitude phenomena. In theme-1, a study has been made on solar variability on middleatmosphere using satellite data and model simulations. The satellite data from UARS-HALOE xperiment show apeak solar response of 4% in ozone and 1 eg.K in temperature per 100 sfu in the lower stratosphere with heightdependence significantly at variance with 2D model simulations. Two multi-instrumented campaigns, one under'space weather' and the other on 'tides' under atmospheric coupling processes, were conducted during March-April2006. The highlights of the campaigns include: improved prediction of the equatorial spread-F based on a newfactor, combining the strength and asymmetry of the EIA; simultaneous detection of quasi two-day wave at bothEEJ and F region heights; omographic image showing TID in association with a counter electrojet event; anunusual owering of mesospheric temperature during a moderate geomagnetic storm; diurnal tide showing a peakamplitude of 35 m/s at 45 km in the zonal wind and a significantly lower amplitude (~10 m/s) in the meridionalwind; and evidence of lower atmospheric convective activity influencing the tidal variability in the MLT region.Under space climate, multiple regression analysis based models for low latitude ionosphere, using Indianionosonde network data taken over three solar cycles, have been developed and found to be a better fit comparedto the commonly used international Reference Ionosphere (IRI).

- 17 -

SA12I-1

Sun-Earth Coupling by Energetic ParticlesCora E. Randall1, Scott M. Bailey3, V. Lynn Harvey1, Charles H. Jackman5, Hanli Liu2, Daniel R. Marsh2, Michael Mills1, and David E. Siskind4

1. University of Colorado, Boulder, CO 80309, USA2. National Center for Atmospheric Research, Boulder, CO 80307, USA3. Virginia Tech, Blacksburg, VA 24061, USA4. Naval Research Laboratory, Washington, DC 20375, USA5. Goddard Space Flight Center, Greenbelt, MD 20771, USA

This talk reviews our understanding of the effects of energetic particle precipitation on the atmosphere. Theemphasis is on interannual variability in these effects as related to solar and geomagnetic activity and atmosphericmeteorology. Energetic Particle Precipitation (EPP) leads to production of NO and NO2 (NOx) from thethermosphere down to the stratosphere. NOx produced above the stratosphere can descend into the stratosphereduring the polar night, given appropriate meteorological conditions. Since NOx is the primary ozone loss catalyticcycle in the middle stratosphere, understanding its source from EPP is critical to interpreting stratospheric ozonevariability. We refer to the phenomenon of NOx production by EPP, followed by transport and chemistry,redistribution of stratospheric ozone, and any subsequent dynamical effects, as Sun-Earth Coupling by EnergeticParticles (SECEP). SECEP varies significantly over the solar cycle, with different characteristics in the northernand southern hemispheres. New observational and modeling results challenge the conventional understanding thatSECEP should be more significant in the southern hemisphere, and generally proportional to the level of EPP.Rather, these studies begin to illuminate the important role of atmospheric meteorology in controlling SECEP. Inthis talk, the most recent advances regarding SECEP will be described, and outstanding questions that must beanswered to gain a comprehensive understanding of these heliophysical pathways to atmospheric coupling will behighlighted.

SA12I-2

Cosmic Rays and ClimateTorsten Bondo

Center for Sun-Climate Research, Danish National Space Center, Danish Technical University, Juliane Maries Vej 30,DK-2100 Copenhagen, Denmark

This work aims to improve our understanding of the role cosmic ray induced ionization has on cloud propertiesand to quantify the resulting climate response. Galactic Cosmic Rays has been studied since the creation of the first electrometers early in the 20th century andprimarily consists of a flux of very high energy charged particles that originate from galactic processes. In theupper atmosphere of the Earth cosmic rays collide with atmospheric nuclei and create a cascade of chargedparticles that are the main source of ionization in the lower part of the atmosphere (below 35 km). The number ofcosmic rays entering the Earth's atmosphere is modulated by both the solar wind and the Earth's magnetic field.The solar wind shields the Earth from galactic cosmic rays such that a weaker field allows for higher GCR fluxes. It was already suggested back in 1959 by Ney that ionization from GCR is the variable of the lower atmospheresubject to the largest solar cycle modulation. However, it wasn't until 1996 that a significant correlation wasidentified in the atmosphere between GCR and the total cloud cover over the solar cycle period (11 years). Thiscorrelation was subsequently shown to be restricted to low clouds, which has important implications forunderstanding the radiative impact on Earth's climate. Clouds play an important role in the Earth's radiationbudget by both reflecting incoming short wave radiation from the Sun and trapping outgoing long wave radiationfrom the surface and lower atmosphere. Low clouds cool the atmosphere, thus the observations suggests that anincrease in GCR leads to an increase in the amount of low clouds resulting in a cooling of the atmosphere. Thisradiative response is consistent with a number of studies demonstrating a correlation between GCR and climateover many time scales from the 11 year solar activity cycle to geological processes over millions of years.However, it remains to be confirmed what the underlying physical mechanism is for this connection.

- 18 -

Recent experimental results from the CSCR experimental facility SKY support the existence of a connectionbetween cosmic rays and the properties of low clouds. The results indicate that ions play a role in nucleating newparticles in the atmosphere and that the rate of production is sensitive to the number of ions and take place onshort time scales. If this sensitivity is relevant for Cloud Condensation Nuclei (CCN) it could provide a possible link between ionscreated by cosmic rays and cloud production.

SA12I-3

Global Electric Circuit Linking Solar Activity and Cosmic Rays to Cloudsand ClimateBrian A. Tinsley

Center for Space Science, WT 15, University of Texas at Dallas, Richardson, TX 75083-0688

There is now strong evidence that the ionosphere-earth current density Jz affects cloud microphysics withconsequences for weather and climate. Jz is modulated regionally by a number of solar and solar wind inputs, bothwithout and with accompanying cosmic ray flux changes. Jz also varies globally with the total output of theatmospheric upward current generators. Observations show clear correlations with Jz of changes in cloud or associated meteorological parameters such aspressure, temperature, or dynamics, for at least 5 disparate sets of such solar and internal atmospheric events thatmodulate Jz. Theory suggests that the space charge generated by Jz in conductivity gradients at the boundaries of layer cloudsaffects rates of scavenging of cloud-condensation nuclei (CCN) and ice-forming nuclei (IFN), that in turn, inseveral different ways, affects drop-size distributions, ice production, precipitation efficiency, and cloud cover. All of the 5 sets of meteorological responses referred to above are short term and do not correlate with total or UVsolar irradiance variations, and 4 of the 5 are independent of cosmic ray flux changes. This makes the Jz/cloudmechanism a necessary and sufficient explanation for these tropospheric responses to solar activity.On the decadal and longer timescales the relative importance of irradiance versus ion-induced nucleation versusthe Jz/cloud mechanisms on tropospheric dynamics has yet to be determined. However, on the multidecadal,millennial, and longer climate timescales the Jz changes at high latitudes are several times larger than on theday-to-day and decadal timescales.

- 19 -

SA12-1

Global Synchronization of Lightning Activity with a Cycle of One MonthYukihiro Takahashi1, Okazaki Yoshitaka1, Mitsuteru Sato 2, Hiroko Miyahara3, Kazuyo Sakanoi4, Toru Adachi1, Hiroshi Fukunishi5, Rue-Ron Hsu6, Han-Tzong Su6, Alfred Bing-Chih Chen6, Stephen B. Mende7, Harald U. Frey7, and Lou-Chuang Lee8

1. Department of Geophysics, Science, Graduate School of Science, Tohoku University, Aramaki, Aoba-ku, Sendai, Miyagi980-8578, Japan2. RIKEN (The Institute of Physical and Chemical Research), 2-1 Hirosawa, Wako, Saitama 351-0198, Japan3. Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku,Tokyo 113-0033, Japan4. Department of Natural Sciences, Komazawa University, 1-23-1 Komazawa, Setagaya-ku, Tokyo, 154-8525, Japan5. Japan Society for the Promotion of Science6. Physics Department, National Cheng Kung University, Tainan 70148, Taiwan7. Space Sciences Laboratory, University of California at Berkeley, 7 Gauss Way, Berkeley, CA 94720-7450, USA8. National Space Organization, Taiwan, 8F, 9, Prosperity 1st Road, Science-Based Industrial Park, HsinChu City, Taiwan,R.O.C.

Although the optical detectors onboard the earth-orbiting satellites, such as OTD or LIS/TRMM, have beenmeasured global lightning activity quite successfully, the day-to-day variations are not well understood because ofthe limited observation frequency at same local time and longitude. We examined the day-to-day lightning activitymodulation based on ELF Schumann resonance measurement. It was reported by Tohoku University group thatthe radiation power in ELF range shows clear peak at about 27-day, the solar rotation period. They confirmed thatthis variation is not caused by the conditions of the ionosphere, which are strongly affected by solar UV, but bythe lightning activity itself. We investigated the longitudinal distributions of the lightning power on a daily basis,assuming that the same local time dependency of lightning activity in any places. It is found that variations in~30-day period are synchronized at almost all local times without significant phase difference. We also examinedthe lightning flash rate observed by ISUAL onboard FORMOSAT-2 satellite and confirmed that in both regions ofAsia and America the variations show almost same tendency at ~30-day periodicity. There may exist two types of explanations for these facts: Firstly, atmospheric electric currents includinglightning discharge are modulated by variations of atmospheric conductivity, which could be caused by cosmicray precipitation. Secondly, thunderstorm activity itself is modulated in the developing phase.

- 20 -

SA12-2

Response of a Global Circuit Model with Stratospheric Aerosol to SolarActivityLimin Zhou1, Brian A. Tinsley2, and Xiangmin Zheng1

1. Key laboratory of Geo-information Science of Ministry of Education, East China Normal University, #3663 N. ZhongshanRoad, Shanghai, 200062,China2. Center for Space Science, University of Texas at Dallas, Richardson, TX, 75080, USA

The global atmospheric electric circuit is important not only as a product of global thunderstorm activity, but itmay cause climate change itself due to the solar activity, via electrical effects on cloud microphysics, withexternal as well as internal drivers, which depends on the current density Jz flowing downwards from theionosphere to the surface through clouds. There is a need for a new model of the global circuit that moreaccurately treats the temporally and spatially varying responses over the globe of changes in the external (spaceweather) forcing agents, and the internal (aerosol distribution, convective activity) forcing agents, and particularlythose that are most important for the temporal and regional variations of Jz, although there are several previousmodels from Hays and Roble (1979); Roble and Hays (1979); Makino and Ogawa (1985); and Sapkota andVarshneya (1990).The purpose of this work is to improve on the treatment of the different and varying aerosol populations, thevarying galactic cosmic ray flux due to the solar activity, and the effects of explosive volcanic eruptions onstratospheric aerosols and stratospheric conductivity.

SA12-3

Cosmic Rays and Variations of Aerosol Optical DepthIrina A. Mironova

Institute of Physics, St.Petersburg State University, Ulyanovskaya 1, Petrodvotets, St.Petersburg, 198504, Russia

One of the main questions which is interested to the CAWSES community is the possible impact of cosmic rays ofsolar and galactic origin on Earth's atmosphere and climate. Here we investigated one of the mechanisms that relay (solar and galactic) cosmic rays variability and opticalatmospheric changes. This link seems to be of great importance for the overall solar-terrestrial relationships. Evena small deviation in the optical properties of the atmosphere can shift the balance between absorption,transparency and albedo. This gives a physically motivated scenario for an enhanced triggering effect of solaractivity on the Earth atmosphere. The objective of our investigation is analysis of the effect of short- (some days) term variations of solar andgalactic cosmic rays on the optical properties of aerosol and atmospheric optical depth. It is taking into accountsolar proton events, ground level effects of solar protons and Forbush decreases of galactic cosmic rays. Theresults explain how strong are the optical atmospheric parameters response to the solar/cosmic signals, how stableare these relationships (both spatially and temporarily) and whether they are affected by other external forces.

- 21 -

SA12-4

Laboratory Studies of the Atmospheric Photodissociation Processes LargelyAffected by Intensity Variations of Solar Ultraviolet Radiation during SolarCyclesKenshi Takahashi1, Tomoki Nakayama2, and Yutaka Matsumi2

1. Kyoto University Pioneering Research Unit for Next Generation, Kyoto University, Gokasyo, Uji, 611-0011 JAPAN2. Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, JAPAN

Although changes of the solar radiation intensity in the visible wavelength region are very small during solarcycles and in long-term variations of the solar activity, they are very large in the vacuum ultraviolet (VUV)wavelength range. The photochemical processes of atmospheric molecules in the VUV wavelength region havenot been well understood due to the experimental difficulties. We are attempting to clarify the interactionprocesses by using laboratory experiments for contribution to model calculations in order to reveal the effect ofintensity variations in solar VUV radiation, which is a remarkable expression of solar activity variation. Wedeveloped a system to detect electronically-excited oxygen atoms O(1S) and nitrogen atoms N(4S) with highsensitivity using vacuum-ultraviolet lasers. In laboratory experiments using this system, we refined the process ofphoto-dissociation of ozone O3 at the wavelength range of 193-230 nm and determined the quantum yield ofO(1S), which is produced in this process. We clarified the reaction process of O(1S) atoms in the stratosphere,mesosphere and lower thermosphere. In the production processes of OH radicals which affect the ozoneconcentration in the stratosphere, the contribution of the O(1S) + H2O reaction process was estimated to be fairlylarge. We also refined the process of photo-dissociation of nitrous oxide N2O at a wavelength of 193 nm anddetermined the quantum yield of N(4S), which is produced in this process. In addition, we clarified the process ofcollision relaxation of rapid N(4S) atoms, which affects the production of nitrogen oxide (NO) in the lowerthermosphere. These data help to clarify the chemical processes concerning to ozone and nitrogen oxides in theupper atmosphere.

SA12-5

Can We Empirically Distinguish Solar from Anthropogenic Forcing ofClimate?Joan Feynman1, Alexander Ruzmaikin1, and Yuk L. Yung2

1. Jet Propulsion Laboratory, California Institute of Technology , Pasadena, California, USA2. Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA

The Earth's climate during the last 100 years is believed to have responded both to solar variability and toanthropogenic forcing. It has been suggested that at the beginning of the 20th century the solar effects were moreimportant than the anthropogenic effects but that in the last few decades the anthropogenic influences havedominated. Is it possible to empirically distinguish between these two forcings of climate? We examine the proposition thatchanges in the solar output cause a surface temperature response pattern in which some large sub-continental areasare cooler while others are warmer than global mean temperature. For example, during the solar-driven MaunderMinimum climate change Northern Europe had cooled and the Middle East had warmed. In contrast,anthropogenic forcing caused warming almost throughout the entire globe. This empirical difference apparentlyreflects a difference in the physical processes involved. Whereas greenhouse gases change the radiative balance,solar output changes affect the occupation frequency of the Annular Modes of the Earth's atmosphere.

- 22 -

SA21I-1

Effect of Variable Schwabe/Hale Cycles of the Sun on Climate ChangeHiroko Miyahara1, Yusuke Yokoyama1, Kimiaki Masuda2, Kentaro Nagaya2, Kyouhei Kitazawa2, Yasushi Muraki2, Hiroyuki Kitagawa3, and Toshio Nakamura4

1. Department of Earth & Planetary Science, University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan2. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan3. Graduate School of Earth and Environmental Sciences, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601,Japan4. Center for Chronological Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan

Measurements of radiocarbon content in tree-rings with annual time resolution enable us to examine the history ofthe Sun and the incoming Galactic Cosmic Rays to the earth. The variations of the radiocarbon content obtainedso far have revealed the variability of the "11-year" and "22-year" cycle of the Sun and the GCRs during the last1200 years. Dendro-chronology data and the oxygen isotopes in ice cores, on the other hand, provide thevariations of temperatures in the past, and the series of data have been obtained by several groups for almost thesame era. By comparing these climate data with the history of the Sun, we have investigated the features of solarinfluence on climate on the multi decadal time scales, and have discussed the possible mechanism of theirrelations. Among the several candidates for the intermediate of Sun-Climate connection, only the Galactic ComicRays retain permanent 22-year cyclicity according to the periodic polarity change of the Sun in every 11 years.The results of spectral analyses of temperature data manifest significant "22-year" periods, but with slightlylonger/shorter lengths according to the changes of solar cycles. It is known that the phases of the "22-year" cyclein GCRs change depending on the level of long-term solar activity. We have found the phase transitions of"22-year" cycle also in temperatures, suggesting that the GCRs is taking more important role in climate change onmulti-decadal time scales rather than the irradiative outputs of the Sun.

SA21I-2

Coupled Chemistry Climate Model Simulations of the Solar Cycle in Ozoneand TemperatureJohn Austin

Geophysical Fluid Dynamics Laboratory

The 11-year solar cycles in ozone and temperature are examined using new simulations of coupled chemistryclimate models. The results show a minimum in lower stratospheric tropical ozone, in agreement with satelliteobservations and in contrast with most previously published simulations. It is found that this improved agreementoccurs by incorporating time varying solar fluxes and sea surface temperatures in the models. The mean modelresponse varies by up to about 2.5% in ozone and 0.8K in temperature during a typical solar cycle. Neither theupper atmospheric effects of energetic particles nor the presence of the quasi biennial oscillation is necessary tosimulate the observed low latitude minimum in lower stratospheric ozone response. Comparisons are also madebetween model simulations and total column ozone. As in previous studies, the model simulations agree well withobservations. However, a substantial difference exists between the observed signal for the period 1960-1980 andfor the period 1980-2000. This is reproduced by those models which cover the full temporal range, and it is shownthat the difference between the solar cycles in the simulations is due almost entirely to ozone changes below 50hPa. Possible reasons for the tropical ozone minimum, and for the difference in ozone response for different solarcycles are discussed.

- 23 -

SA21I-3

Observations and Modelling Studies of the 11-year Solar Cycle in the LowerStratosphereLesley J. Gray, Stephen T. Rumbold, and Keith P. Shine

Meteorology Department, University of Reading, U.K.

In addition to the well-known 11-year solar cycle temperature response at the equatorial stratopause, there is asecondary response in the lower stratosphere that is not well reproduced by most model studies. An ability toreproduce this feature is important in order to successfully model the transfer of the solar cycle signal to thetroposphere and hence the Earth's climate. The observations of the 11-year solar signal in the lower stratospherefrom analyses of ERA-40 and SSU/MSU data will be reviewed. The relative contributions of (a) solar irradiancechanges and (b) associated ozone changes to the lower stratosphere signal will be examined, using a fixeddynamical heating model. Model experiments in which these two factors are included separately and then togetherwill be described. The imposed ozone changes are taken from a regression analysis of satellite observations(Randel and Wu, 2007). The model reproduces the observed temperature response very well, in contrast to earlierstudies that employed ozone distributions from simple 2-d model predictions (Shibata and Kodera, 2005). Theresults suggest that the 11-year solar cycle signal in ozone is the prime cause of the lower stratosphere temperaturesignal. Although the fixed dynamical heating formulation excludes direct dynamical influences on temperature,circulation changes are nevetheless the prime factor that determine the ozone changes in this region of theatmosphere. A major conclusion of this study is therefore that coupled chemistry models will need a goodsimulation of lower stratospheric dynamics if the model is to successfully reproduce the 11-year solar signal in theequatorial lower stratosphere.

SA21-1

Creation of a Composite Solar Ultraviolet Spectral Irradiance Data SetMatthew T. DeLand and Richard P. Cebula

Science Systems and Applications, Inc. (SSAI), Lanham, MD 20706, USA

Solar ultraviolet (UV) irradiance is deposited in the atmosphere at altitudes ranging from the lower stratosphere tothe lower thermosphere. Understanding the spectral and temporal dependence of solar UV variations is thuscritical to characterizing the long-term terrestrial energy input over a wide vertical region. Regular spectral solarUV measurements from space began in late 1978 with the Nimbus-7 SBUV instrument, and have continued to thepresent using overlapping data sets from multiple instruments (SME, SBUV/2 on NOAA satellites, SUSIM andSOLSTICE on UARS). However, wavelength-dependent absolute biases and drifts are observed when any twodata sets are compared. We have developed a composite spectral irradiance data set covering the wavelengthrange 120-400 nm for the period 1978-2004 as part of the NASA Living With a Star program. We will describethe methods used to evaluate and merge the individual data sets, and discuss the quality and limitations of the finalirradiance product. We intend to extend our composite UV irradiance data set into the future using data from theSOLSTICE and SIM instruments on the SORCE mission.

- 24 -

SA21-2

Solar Modulation of the Recent Trends in the NH Winter CirculationKunihiko Kodera1, Masatake E. Hori1, Seiji Yukimoto2, and Michael Sigmond3

1. Graduate School of Environmental Studies, Nagoya University, Nagoya, Japan2. Meteorological Research Institute,Tsukuba, Japan3. School of Earth & Ocean Sciences, University of Victoria, Victoria, Canada

It was suggested that the recent winter warming of the NH is due to the increasing trends of the North AtlanticOscillation (NAO) or the Arctic Oscillation (AO). However, previous studies showed that the spatial structure ofthe NH winter teleconnection pattern related to the NAO are different according to the solar activity. An AO-likehemispherical structure preferentially appears during high solar activity. Therefore spatial structure of the recenttrend could be changed according to the solar activity. In fact, the trends in the sea level pressure (SLP) during high solar (HS) activity exhibit NAO/AO-like patternconnected to a stronger stratospheric polar vortex, whereas during low solar (LS) activity decreasing trends in theSLP appear over the north-eastern Pacific region in association with warming trends in the tropical troposphere.These two trends compare well with those found in numerical model simulations where the CO2 was doubled ineither the troposphere or the middle atmosphere. The result of the present study suggests that the cooling effect ofthe middle atmosphere due to increased CO2 can penetrate into the troposphere during HS winters.

SA21-3

Simulation of the Effect of 11-year Solar Cycle with MRIChemistry-Climate ModelKiyotaka Shibata and Makoto Deushi

Meteorological Research Institute

It is well known that the 11-year solar cycle is the most prominent cycle giving rise to large impacts on thestratospheric temperature and ozone through substantial irradiance variations of about several % at UVwavelengths. Though the total solar irradiance variation of the 11-year solar cycle is at most 0.1 %, its signal canbe evidently detected from the upper stratosphere down to the surface in the observed geopotential data. Indeedthe 11-year solar cycle effect on the upper stratosphere is straightforward enough to be readily understood as adirect result of the UV irradiance changes, but its indirect effect through dynamics on the lower stratosphere is notnecessarily well clarified as for the mechanism. In this study, the 11-year solar signals were inve stigated in thesimulation of Meteorological Research Institute chemistry-climate model (MRI-CCM), which was driven byobserved forcings for the recent past 1980-2004. MRI-CCM is based, for a dynamical module, on a MJ98 GCMwith an eta-ordinate [Shibata et al., 1999]. To reproduce the quasi-biennial oscillation (QBO) in the tropicalstratosphere, the non-orographic gravity wave drag (GWD) scheme of Hines [1997] is incorporated with enhancedgravity wave source over the tropics, instead of Rayleigh friction. In addition, the biharmonic horizontal diffusionis weakened in the middle atmosphere, where the e-folding time at the maximum wavenumber 42 is set at 150 hrs,being slightly less than the previous value of 180 hrs [Shibata and Deushi, 2005a]. The chemical module includes36 long-lived and 15 short-lived species with 80 gas-phase reactions, and 35 photodissociations with 9heterogeneous reactions. MRI-CCM has a horizontal resolution of 2.8 by 2.8 degrees (T42) in longitud e-latitudespace and has 68 layers (L68) extending from the surface to the mesopause (~0.01 hPa) with 500m verticalspacing from 100 to 10 hPa. MRI-CCM adopts a hybrid semi-Lagrangian transport scheme, in which a new PRM5scheme is developed by improving both vertical and horizontal procedures to simulate better distributions of

- 25 -

chemical constituents; the vertical procedure employs the piecewise rational method (PRM) [Xiao and Peng,2004] and the horizontal procedure uses a quintic interpolation. Ensemble CCM simulation was made under theCCMVal REF1 scenario [Eyring et al., 2005], in which both natural and anthropogenic forcings of SST, sea-ice,greenhouse gases, halogens, the 11-year solar cycle, and volcanic aerosols are given daily through interpolationfrom monthly mean values. The integration period covers the period from November 1979 to December 2004,prior to which spin-up integration was made for more than several years. The general conditions of the REF1 aredescrib ed in Eyring et al. [2005]. There are two giant volcanic eruptions, El Chichn (7.4N, 93.2W) inMarch/April 1982 and Mount Pinatubo (15.1N, 120.4E) in June 1991, over the entire integration period. Linearmultiple regression analysis is used to isolate specific signals from the anomalies in temperature and ozone datafor the simulation and observations. Reference variables are the mean value, the linear trend, the QBOs at 20 and50 hPa, volcanic aerosols of El Chichn and Mount Pinatubo , El Nio/Southern Oscillation (ENSO), and the11-year solar cycle. It is found that MRI-CCM can more or less realistically reproduce observed trend ofannual-mean temperature and ozone. The annual-mean QBO signals of temperature and ozone is well reproducedas for the meridional structures. The seasonality of the mid-latitude total ozone QBO is also quantitativelyreproduced including extensions to hi-latitudes in winter hemispheres. The vertical three-cell of alternatin g sign(positive in the upper stratosphere, negative in the middle stratosphere, and positive in the lower stratosphere) inthe tropical stratospheric temperature due to the 11-year solar cycle is qualitatively reproduced. On the other hand,the simulated ozone reproduced positive signals in the upper and lower stratosphere, but did not exhibit negativesignal in the middle stratosphere.

SA21-4

Parameter Sweep Experiments on Remote Influences of QBO and SolarCycle with a Simple Global Circulation ModelKosuke Ito, Yoko Naito, and Shigeo Yoden

Department of Geophysics, Kyoto University, Kyoto 606-8502, JAPAN

The combined effects of the quasi-biennial oscillation (QBO) and the 11-year solar cycle on the global circulationare investigated in a series of numerical experiments with a simple global circulation model under a perpetualwinter condition. A zonal momentum and temperature anomalies are introduced to mimic a phase of the QBO andthe 11-year modulations of temperature field around the stratopause, respectively. The QBO phase, and theintensity and location of the temperature increase due to the solar forcing are swept as experimental parameters.The datasets obtained from 10,800-day integrations for 66 runs are analyzed statistically for a large number ofsamples. In the group of the QBO westerly runs, the time-mean stratospheric temperature at the North Pole is significantlyhigher in solar-max forcing when the latitudinal temperature gradient by the solar forcing difference is located inmid-latitudes of the winter hemisphere, while the result is reversed when the gradient is located in low-latitudes orthe summer hemisphere. In the group of the easterly runs, the time-mean stratospheric temperature at the NorthPole is lower in the solar-max runs regardless of the solar forcing location. In case that the latitudinal temperaturegradient is located in mid-latitudes of the winter hemisphere, the combined effects of the QBO and the solarforcing on the polar stratosphere in winter are consistent with the observational studies by Labitzke (1987) andLabitzke and van Loon (1988).The solar effect in the present experiments is seen in the anomaly of Eliassen-Palm flux around the stratopause.The temperature changes in the polar stratosphere are consistent with this anomaly through the downward controlprinciple. Similarity to the observed relationship is discussed in terms of the dynamics of planetary waves.

- 26 -

SA21-5

Tidal Waves in the Stratosphere and Lower Mesosphere as Inferred FromCCM SimulationsMisako Kitamura1, Toshihiko Hirooka1, Kiyotaka Shibata2, and Hideharu Akiyoshi3

1. Department of Earth and Planetary Sciences, Kyushu University, Hakozaki, Fukuoka 812-8581, Japan2. Meteorological Research Institute, Nagamine, Tsukuba 305-0052, Japan3. National Institute of Environmental Studies, Onogawa, Tsukuba 305-8506, Japan

Atmospheric tides are mainly forced by diurnal variations of the heating due to absorption of solar radiation byozone and water vapor. Features of atmospheric tides in the stratosphere and lower mesosphere and theirmodulation due to the solar cycle are examined by the use of coupled chemistry-climate models (CCMs) withsophisticated stratospheric chemistry developed at the Center for Climate System Research of the University ofTokyo (CCSR) / National Institute of Environmental Studies (NIES) and Meteorological Research Institute(MRI). Results show that in both simulations diurnal tides are clearly seen in summer hemispheres of thestratosphere and lower mesosphere. The global structure is identifiable with the gravest external mode of diurnaltides based on the classical tidal theory. As regards the ozone field, corresponding diurnal components are alsopredominant with two maxima around 1 hPa and 5 hPa at latitude 70 degrees in summer hemispheres, whichtravel westward behind the sun by about 13 hours and 5 hours, respectively. However, the formation mechanismis still unknown and further studies are needed. Daily changes of tidal waves are relatively small in the summerhemispheres and larger amplitudes are seen in the solar maximum simulation almost throughout the period.

- 27 -

SA22I-1

Diagnosing the Response of the Stratosphere to the 11-year Solar CycleAnne K. Smith1 and Katja Matthes2

1. National Center for Atmospheric Research, Boulder CO 80307, USA2. Free University of Berlin, Berlin D-12165 Germany

An interactive 2-dimensional model is used to explore aspects of diagnosing the stratospheric response to the solarcycle. The model includes time-dependent forcing of solar flux variations and of momentum forcing forsimulating the Quasi-Biennial Oscillation (QBO) in stratospheric winds.. A number of model simulations includedifferent QBO and solar flux time series. The analyzed response of stratospheric ozone and temperature to thesolar cycle is different in each simulation, even with a data record of four solar cycles (~43 years). In general, twofeatures are found. 1) Statistically removing the impact of the QBO from the analyzed solar response is moresuccessful with sinusoidal QBO forcing than with QBO forcing based on observations but not complete in eithercase. 2) The response of both ozone and temperature to solar flux variations is substantially larger when the solarflux varies smoothly (either sinusoidal or 12-month smoothing) than for the highly variable monthly averagedvariations. These results indicate that one should use caution in the interpretation of the response of thestratosphere to the solar cycle from the limited observational record currently available.

SA22I-2

Solar Cycle Influences on the Stratosphere and Implications for theTropospheric Circulation over EuropeKleareti Tourpali1 and Cornelius J. E. Schuurmans

1. Laboratory of Atmospheric Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece2. Institute for Marine and Atmospheric Research, Utrecht University, The Netherlands

The 11-year solar cycle influence on stratospheric dynamics and its effects on the North Atlantic Oscillation areinvestigated with a coupled Chemistry-Climate Model. A structural modulation is found with its main featuresbeing an eastward shift of the surface Atlantic center of action into Europe and a vertical extension into thestratosphere during solar maximum conditions. These results are in good agreement with observation analysis ofthe ERA-40 and NCEP-Reanalysis data sets. As the above results suggest a solar effect in the troposphericcirculation, the solar cycle modulation of the northern hemisphere atmospheric blocking is examined and aninfluence is found in the Euro-Atlantic Region

- 28 -

SA22-1

Forcing of the Earth's Atmosphere by Solar RadiationKlemens Hocke and Niklaus Kaempfer

Institute of Applied Physics, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland

The changing Sun-Earth distance induces an annual variation of total solar irradiance (TSI) with an amplitude of 45.7 W/m^2 at the place of the Earth. This is much larger than the other variations of TSI, e.g., the 11-year solarcycle corresponds to an amplitude of around 1 W/m^2. We estimate the impact of the annual variation of TSI on the time series of global mean temperature at differentaltitudes by assuming radiative equilibrium. Then we search for signatures of the solar radiation forcing in atmospheric data from NCEP/NCAR reanalyses and the empirical climatology NRLMSISE-00 (major upgrade ofMSIS-90). Generally, inter-hemispherical asymmetries of the atmospheric water vapor distribution mask the effect of thechanging Sun-Earth distance. The role of water vapor for the thermal state and the circulation of the atmosphere is discussed as well as globaland hemispherical trends of temperature, water vapor, and pressure.

SA22-2

Sensitivity of the 11-year Solar Signal to Changes in Ultraviolet Radiationand OzoneUlrike Langematz and Katja Matthes

Institut fuer Meteorologie, Freie Universitaet Berlin, Carl-Heinrich-Becker-Weg 6-10, 12165 Berlin, Germany

We present results from a series of multi-annual sensitivity simulations with the Freie University Berlin-ClimateMiddle Atmosphere Model (FUB-CMAM) in which we systematically prescribed either changes in ultraviolet(UV) radiation or ozone between solar minimum and maximum, or different combinations of both forcings, tostudy their relative impact on the thermal and dynamical structure of the stratosphere and mesosphere. Thesimulations were integrated for perpetual solar maximum and minimum conditions, each over 50 years to excludepotential disturbing effects from natural interannual dynamical variability in the northern winter stratosphere.Our results suggest that in the summer hemisphere during solstice, both UV and ozone changes are of equalrelevance for the short-wave (SW) heating rates and the temperature signal in the stratosphere. While the impactof the UV changes dominates in the upper stratosphere and mesosphere, the ozone changes determine the solarheating rate and temperature signal in the lower stratosphere. All simulations show a warming of the stratosphere,consistent with the SW heating rate changes. However in the winter hemisphere, larger and robust negativetemperature changes occur as a result of dynamical changes due to changes in planetary wave dissipation andmodifications of the meridional residual circulation.

- 29 -

SA22-3

Solar Cycle Modulation of the Troposphere-Stratosphere Coupling in theSouthern Hemisphere WinterYuhji Kuroda, Makoto Deushi, and Kiyotaka Shibata

Meteorological Research Institute, 1-1 Nagamine, Tsukuba, 305-0052, JAPAN

The effect of the 11-year solar cycle on the troposphere-stratosphere (TS) coupling in the southern hemisphere(SH) late winter is examined through the analysis of observations and simulations with a chemistry-climatemodel. It is found that the TS coupling in the SH late winter is largely modified according to the solar cycle; thedynamical coupling between the troposphere and stratosphere becomes stronger with the increasing solar activity.Such modulation of the strength of the TS coupling is found to be the source of the solar-cycle modulation of theannular mode in late winter.

SA22-4

The Role of The QBO in Simulating the Silar Signal in the AtmosphereKatja Matthes1, Rolando R. Garcia2, Daniel R. Marsh2, and Anne K. Smith2

1. Institut fuer Meteorologie, Freie Universitaet Berlin, Berlin, Germany2. National Center for Atmospheric Research, Boulder, USA

The 11-year solar cycle has an impact on the chemical, thermal, and dynamical structure of the atmosphere.Observational and modeling studies have shown that direct radiative changes in the upper stratosphere can lead toindirect dynamical changes throughout the atmosphere. However, the understanding of the interaction with theequatorial stratospheric Quasi-Biennial Oscillation is still a challenging topic. Discrepancy exists in separating thesolar and QBO signals in observations partly due to the short length of existing data sets. Therefore modelingstudies are useful to enhance the understanding of the underlying physical mechanism(s). To understand the response of the middle atmosphere to the 11-year solar cycle and its possible transfer to thetroposphere a comprehensive set of experiments made with a state-of-the-art chemistry climate model thatincorporates the whole atmosphere up to the thermosphere will be investigated. Especially the role of anexternally prescribed stratospheric QBO in influencing the 11-year solar cycle signal in NCARs WholeAtmosphere Community Climate Model (WACCM3) will be discussed. The set of experiments with WACCM3 consists of different perpetual condition experiments (solar cycle only orsolar cycle and QBO) with different horizontal resolutions as well aslong-term 110-year sensitivity experiments, in which only a realistic time varying solar cycle, only a synthetic,time varying QBO or both the solar cycle and the QBO, were included. In all simulations the sea surfacetemperatures had a repeating climatological seasonal cycle and the greenhouse gases were set constant to 1995conditions. We will show and discuss differences in the solar signals in the QBO east and west experiment that are inagreement with several observational studies.

- 30 -

SA22-5

Solar Cycle Modulation of Wave Forcing over Troposphere Related to theAnnular Mode over StratosphereYousuke Yamashita and Masaaki Takahashi

Center for Climate System Research, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, 277-8568, Japan

The energy flux of high energy UV radiation changes by large (>5%) amounts during the 11-year solar cycle. Thetemperature in the stratosphere is affected by the direct radiation, while the lower atmosphere can be influencedthrough the interaction with dynamics (Kuroda and Kodera, 2002). The winter (DJF) mean 10.7cm solar radio flux is used for evaluation of solar activity. Based upon the wintersolar activity, we divide all years into high solar (HS) and low solar (LS) period. The Empirical OrthogonalFunction (EOF) decomposition is applied over stratosphere, and we derive the principal component (PC)time-series of the EOF-1 in December. Data used in the EOF decomposition originate from the NCEP/NCARreanalysis monthly mean geopotential height fields for 1979 to 2005.The zonal mean zonal wind is regressed to the PC 1 over stratosphere in December. In the HS, the westerly windanomaly at 60 N extends from the stratosphere to the troposphere. The westerly wind anomaly over thetroposphere is maintained largely by wave forcing term, and the wave forcing term over troposphere is strong inHS and weak in LS. The result indicates that the wave forcing term is important factor to the solar cyclemodulation of the westerly wind anomaly in the troposphere. The stationary component is large contribution to thewave forcing term, and the transient component is significant contribution.

SA22-6

Effects of the 11-year Solar Cycle on Mid-tropospheric Circulation in theNorthern Hemisphere in WinterRadan Huth1, Josef Bochnicek2, Lucie Pokorna1, Jan Kysely1, Romana Beranova1, and Pavel Hejda2

1. Institute of Atmospheric Physics, Bocni II 1401, 141 31 Praha, Czech Republic2. Institute of Geophysics, Bocni II 1401, 141 31 Praha, Czech Republic

We examine the solar activity effects on various aspects of tropospheric circulation in the Northern Hemisphere.The analysis concerns winters in 1950-2003. Analyzed are monthly mean values. Solar activity is characterized bythe 10.7 cm radio flux. Separate analyses are conducted for low, moderate, and high solar activity. Troposphericcirculation is described by modes of low-frequency variability (teleconnections); teleconnectivity, i.e., maximumnegative spatial autocorrelations; correlations between the variability modes and surface temperature andprecipitation in Europe; stormtracks; and frequency of synoptic types according to Hess-Brezowsky (defined overEurope). Data used are 500 hPa heights from the NCEP/NCAR reanalysis. Statistically significant differencesbetween solar maxima and minima appear for all the circulation characteristics, e.g. in the position and intensityof the action centres of the variability modes, intensity of stormtracks, and the frequency of groups ofHess-Brezowsky synoptic types. A general effect is that under a high solar activity, the circulation tends tozonalize and the geographical extent and influence of the modes are larger. One of the effects of a high solaractivity is a tendency towards splitting the NAO. Some effects, e.g., the activization of the North Asian mode, arepronounced for a moderate solar activity, which poses a warning that in investigations of solar effects on thetroposphere, one should not rely on the extremes of the solar cycle only, but should consider the non-extremephases as well.

- 31 -

SA31I-1

Lower Atmospheric Sources of Longitudinal Variability in the QuiescentIonosphereMaura E. Hagan, Astrid Maute, Raymond G. Roble, and Arthur D. Richmond

High Altitude Observatory National Center for Atmospheric Research, Boulder, Colorado, USA

We report on a numerical investigation into the effects of nonmigrating tides on the Earth's ionosphere, which weconducted with the thermosphere-ionosphere-mesosphere-electrodynamics general circulation model(TIME-GCM). Our results extend the recent work of Hagan et al. (2007) who demonstrated that longitudevariations in IMAGE satellite airglow brightness measurements associated with equatorial ionization anomalypeak densities can be attributed to longitudinally variable zonal wind perturbations which modulate the E-regiondynamo and produce electric field effects that map into the F-region aloft. In this presentation we further explorethe nonmigrating tidal components that can produce such lower thermospheric zonal wind perturbations andplausible sources, including latent heat release associated with raindrop formation in deep convective towers inthe tropical troposphere. We also report on whether and how TIME-GCM ionospheric longitude variations evolvewith altitude, local time and season, making comparisons with observations, as appropriate.Hagan, M.E., A. Maute, R. G. Roble, A. D. Richmond, T. J. Immel, and S. L. England, (2007),Connections between deep tropical clouds and the Earths ionosphere, Geophys. Res. Lett., in press.

SA31I-2

Results from the CAWSES Global Observing Campaign on TidesWilliam E. Ward and CAWSES Tidal Campaign Team

Department of Physics, University of New Brunswick, Fredericton, NB, E3B 5A3, Canada

Three global tidal campaigns (September/October, 2005, March/April, 2007 and June/August 15, 2007) and twoworkshops (July, 2006 and August 2007) have taken place over the past two year as part of the CAWSES GlobalObserving Campaign on Tides. The goal of these observations is to provide spatial and temporal samplingsufficient to resolve wavenumbers up to at least 5 and periods down to 4.8 hours every two to three days,something neither satellite observations or ground based observations can do independently. Analyses of thesedata sets provide insights into the character of the tides in and their impact on the terrestrial atmosphere. Thisproject is one of several sponsored under Theme 3, Atmospheric Coupling Processes, of the international Climateand Weather of the Sun Earth System program. During the campaigns observations from a number of instrumentsand types of instruments were taken. These included various types of radars,lidar, optical imagers andinterferometers, ionosondes, magnetometers as well as constituent, wind and temperature measurements fromsatellites. The workshops provided an opportunity for intercomparisons between the various observation types, theidentification of the dominant components and their latitudinal structure and comparisons with models. In this paper, we describe the organization of this effort, describe the observations, associated analyses andcomparisons, initial conclusions and future activities. The CAWSES Tidal Campaign Team: W.E. Ward, Dept. of Physics, University of New Brunswick, Canada; M.Gerding Leibniz-Institute of Atmospheric Physics, Kuhlungsborn, Germany; L. Goncharenko MIT HaystackObservatory, Route 40, Westford, MA 01886 USA; P. Keckhut Service d?fA??±ronomie, Institut Pierre et SimonLaplace, Verri???re-le-Buisson, France; D. Marsh Atmospheric Chemistry Division, NCAR, P.O. Box 3000,Boulder, Colorado 80307-3000, USA; J. Oberheide Physics Department, University of Wuppertal, Wuppertal,Germany; D.N. Rao National Atmospheric Research Laboratory, P.B. No. 123 Tirupati - 517 502, India; J. Scheer

- 32 -

Instituto de Astronom??¿a y F??¿sica del Espacio, Consejo de Investigaciones Cient??¿ficas y T??±cnicas,Universidad de Buenos Aires, Buenos Aires, Argentina; W. Singer Leibniz-Institute of Atmospheric Physics,Kuhlungsborn, Germany; J. Forbes,Dept. of Aerospace Engineering Sciences, Boulder, CO, USA; N. Grieger,Leibniz-Institute of Atmospheric Physics, Kuhlungsborn, Germany; S. Gurubaran, Indian Institute ofGeomagnetism, EGRL,Tirunelveli, India; M. Hagan, High Altitude Observatory, NCAR, Boulder, CO, USA; K.Hamilton, SOEST, University of Hawaii, Hawaii, USA; R. Lieberman, Northwest Research Associates, CoRADivision, Boulder, CO, USA; M. Mlynczak, NASA Langley Research Center, Hampton, VA, USA; T. Nakamura,RISH, Kyoto University, Uji, Japan; J. Oberheide, Physics Department, University of Wuppertal, Wuppertal,Germany; D. Pancheva, Dept. of Electronic & Electrical Engineering, University of Bath, Bath, UK; H.Takahashi, INPE, CP-515, 12245-970 Sao Jose dos Campos, SP, Brasil

SA31-1

Observations of Traveling Atmospheric Disturbances (TADs) inThermosphere Density Using the CHAMP and GRACE AccelerometersSean L. Bruinsma1 and Jeffrey M. Forbes2

1. Department of Terrestrial and Planetary Geodesy, Centre National d'Etudes Spatiales, 18, Avenue E. Belin, 31401Toulouse, France2. Department of Aerospace Engineering Sciences, UCB 429, University of Colorado, Boulder, CO 80309-0429, USA

Accelerometers on the CHAMP and GRACE satellites have made it possible to accumulate near-continuoussimultaneous records of thermosphere density between about 380 and 500 km since March, 2002, and haverecorded the response to virtually every significant geomagnetic storm during this period. The CHAMP andGRACE satellites are in near-polar and quasi-circular orbits, which enable us to derive the thermospheric densityresponse at four local times for each event. These capabilities offer unique opportunities to study the temporal andlatitudinal responses of the thermosphere to geomagnetic disturbances. Data from about 30 geomagnetic storms were explored, but the observed response of the thermosphere to thegeomagnetic storm of 29-30 May 2003 is analyzed in detail. The atmospheric variability is evaluated byde-trending the data and analyzing density 'residuals' corresponding to several ranges of horizontal scale. Thescale of the perturbation is decisive for its lifetime and relative amplitude. Sometimes the disturbances representwave-like structures, and for the May 2003 storm several Traveling Atmospheric Disturbances (TADs) weredetected. Some of these traveled over the pole into the opposite hemisphere, which was never observed so far,while most propagate equatorward. The estimated speeds of the observed TADs are of the order of 400-800 m/s. TADs are relatively rare in the CHAMP and GRACE density multi-year time series, and their detection islaborious. Besides the May 2003 storm period, we found only twelve additional storm events that gave rise tosignificant and unambiguous TAD activity.

- 33 -

SA31-2

The Neutral Wind in the Polar Lower Thermosphere Observed during theStrong Ionospheric ConvectionTakuo T. Tsuda1, Satonori Nozawa1, Shinichiro Oyama1, Tetsuo Motoba2, Yasunobu Ogawa3, Hiroyuki Shinagawa4, and Ryoichi Fujii1

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan2. Graduate School of Environmental Studies, Nagoya University. Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan3. National Institute of Polar Research, 9-10, Kaga 1-chome,Itabashi-ku, Tokyo 173-8515, Japan4. National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795Japan

We analyzed the data obtained on 16 June 2005 with the EISCAT Svalbard Radar at Longyearbyen (78.2 deg N,16.0 deg E, 75.2 deg N invariant latitude) in order to investigate importance of the ion drag on the lowerthermospheric wind dynamics under conditions of strong ionospheric convection (> ~2000 m s-1). On 16 June2005, the ion flow speed in the F region began to increase at ~0900 UT, associated with the southward turning ofIMF observed by the ACE satellite. Between ~1000 UT and ~1300 UT, the speed of ion flow exceeded 1000 ms-1 with the maximum speed of ~3000 m s-1 (equivalent to an electric field of ~150 mV m-1). The increase ofneutral wind velocity was also found between ~1000 and ~1300 UT, and its magnitude exceeded ~500 m s-1 at118 km. The temporal variations of the neutral winds at 113 km and 118 km exhibited similar variations to thoseof the ion flows. One may imagine that the ion drag was a dominant force to accelerate the neutral wind during theperiod. We will present comparison of the acceleration values of total, ion drag, and Coriolis, and discuss theimportance of the ion drag in this event.

SA31-3

Multi-Instrument Observations of F- and E-Region Ionosphere Couplingover JapanMamoru Yamamoto1, Toru Adachi1, Yuichi Aoki1, Akinori Saito2, Yuichi Otsuka3, Susumu Saito4, and Tatsuhiro Yokoyama5

1. Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Kyoto 611-0011, Japan2. Department of Geophysics, Kyoto University, Kyoto 606-8502, JAPAN3. Solar-Terrestrial Environment Laboratory, Nagoya University, Toyokawa, Aichi 442-8507, JAPAN4. National Institute of Information and Communications Technology, Koganei, Tokyo 184-8795, JAPAN5. Earth and Atmospheric Sciences, Cornell University, Ithaca, NY 14853, USA

FERIX (F- and E-Region Ionosphere Coupling Study) is the multi-instrument experiment for electromagneticcoupling processes. The first experiment was done in 2004. By using the MU radar and a portable VHF radar, wesucceeded simultaneous observations of F- and E-region ionospheric irregularities along the same geomagneticfield line. FERIX-2, the second run of the experiment, is conducted in June-September 2007. For this experimentwe apply the radar imaging technique for both radars, and study the coupling processes in more detail. Additionaldata are available from a network of airglow imagers and the GEONET, the GPS receiver network over Japan. Weoverview results from FERIX and FERIX-2, and discuss coupling processes that occur in the mid-latitudeionosphere.

- 34 -

SA31-4

GPS Observations of Ionospheric Irregularities over Indonesia and TheirRelation to Atmospheric Waves from BelowYuichi Otsuka1, Tadahiko Ogawa1, Kazuo Shiokawa1, and Takuji Nakamura2

1. Solar-Terrestrial Environment Laboratory, Nagoya University2. Research Institute for Sustainable Humanosphere, Kyoto University

As part of the CPEA (Coupling Processes in the Equatorial Atmosphere) project, we have conductedmeasurements of 1.6-GHz GPS ionospheric scintillation at Kototabang, Indonesia since 2003 to monitorionospheric irregularities with a spatial scale of about 400 m within equatorial plasma bubbles. Plasma bubbles inthe equatorial F region ionosphere are known to be generated in the bottomside of the F region after sunsetthrough the Rayleigh-Taylor (R-T) plasma instability. However, the seeding processes of plasma perturbationsthat ultimately develop into bubbles through the R-T instability are unknown. To investigate the relationshipbetween bubble occurrences and atmospheric gravity wave (AGW) activity in the troposphere, we analyzed bothGPS ionospheric scintillation index and cloud top temperature (Tbb) over the Indian Ocean measured bymeteorological satellites. The results suggest a meaningful correlation between S4 and Tbb, and that timevariations of S4 and Tbb have common periods of a few to 13 days, perhaps due to planetary waves. S4 was alsocompared with mesospheric neutral winds observed by a meteor radar at Kototabang. The results show thatsemidiurnal variations at the mesosphere may affect the plasma bubble occurrence.

- 35 -

SA32I-1

Up- and Downward Coupling Processes in the HAMMONIA EntireAtmosphere ModelHauke Schmidt1, Guy P. Brasseur2, Marco A. Giorgetta1, Martin Keller1, and Elisa Manzini3

1. Max Planck Institute for Meteorology, 20146 Hamburg, Germany2. National Center for Atmospheric Research, Boulder, CO, USA3. Euro-Mediterranean Centre for Climate Change (CMCC/INGV), Bologna, Italy

It is well known that middle and upper atmospheric layers are strongly influenced from below, in particularthrough upward propagating waves of different types. Possible downward coupling processes are less evident andmore controversely discussed. With the advent of comprehensive general circulation models that encompass theatmosphere from the surface to the thermosphere studies of coupling mechanisms in both directions have beenfacilitated. One of these models is the Hamburg Model of the Neutral and Ionized Atmosphere (HAMMONIA). Inthis paper we present results from two numerical experiments concerning upward and one concerning downwardcoupling. Firstly, we assess the influence of the quasi-biennial oscillation (QBO) of stratospheric winds onmesospheric dynamics, temperature and trace gas concentrations. Secondly, an estimation is given for the part ofmiddle atmospheric variability that is caused by tropospheric forcing versus the part that is of local origin. This isanalyzed from an ensemble of experiments with tropospheric dynamics assimilated to reanalysis data. Besides thiswe present an analysis of the downward coupling mechanism involved in transporting the atmospheric response to11-year solar cycle UV variability from the stratopause region to the tropopsphere.

SA32I-2

Generation of the Thermospheric Localized Structures Simulated by aWhole Atmosphere GCMHitoshi Fujiwara1 and Yasunobu Miyoshi2

1. Deaprtment of Geophysics, Tohoku University2. Department of Earth and Planetary Sciences, Kyushu University

Although the mass density is one of the most important parameters in the upper atmosphere for studies of spaceweather and environment, the details of its localized structures and variations are still unknown. Recently, satelliteobservations have revealed some interesting features of the thermospheric mass density structure, e.g., theequatorial thermospheric mass density anomaly, globally propagating traveling atmospheric disturbances (TADs),and response to the solar flare. In order to investigate global distributions and variations of the thermosphericdensity, temperature, and wind, we perform numerical simulations by using a whole atmosphere generalcirculation model (GCM) [Miyoshi and Fujiwara, 2003]. This GCM describes coupling processes between thelower and upper atmospheric regions and between the high- to low-latitude regions in the thermosphere. TheGCM results show coupling between TADs propagating from high- to low-latitude and the lower atmosphericeffects produces localized disturbances in the mid- and low-latitude thermosphere. In the present study, generationmechanisms of the localized thermospheric structures are investigated. In particular, the production mechanismsof the mass density structure shown by recent observations are discussed.

- 36 -

SA32-1

Radar Observations of Long-term Variability of Mesosphere and LowerThermosphere Winds over TropicsS. Sridharan1, T. Tsuda2, and S. Gurubaran3

1. National Atmospheric Research Laboratory, Gadanki, Pakala Mandal-517 112, Chitoor, India2. Research Institute for Sustainable Humanosphere, Kyoto University, Gokasho, Uji-611 0011, Kyoto, Japan3. Equatorial Geophysical Research Laboratory, Indian Institute of Geomagnetism, Krishnapuram, Tirunelveli-627 011, India

The horizontal wind data acquired by MF radar at Tirunelveli (8.7N, 77.8E) since January 1993, meteor radar atJakarta (6S, 109E) during 1993-1999 and another MF radar at Pameungpeuk (7.5S, 107.5E) since March 2004 areused to study the long-term variability of equatorial mesosphere and lower thermosphere (MLT) winds overtropics. The monthly mean zonal winds over the above tropical sites exhibit dominant semi-annual variation withwestward winds during equinox and eastward winds during solstice. The first westward phase of semiannualoscillation, which occurs during spring equinox, undergoes interannual variability with larger westward windsduring the years 1993, 1995 and 1997. This interannual variability has been interpreted as quasi biennialoscillation (QBO) in the MLT winds. However, the large westward winds, which are expected to occur during theyear 1999, instead occur during the year 2000. Thus the period of QBO is extended from nearly two years to threeyears. During these years, the period of stratospheric QBO winds is also extended to three years. Besides SAOand QBO, as the zonal winds undergo intraseasonal oscillations with periodicities resembling those ofMadden-Julian Oscillation (MJO) in the troposphere, the relation between the two is examined based on theexisting hypothesis. The monthly mean meridional winds undergo annual oscillation, the amplitude of whichenhances in some years when large westward winds are observed. Besides, there is a decreasing trend observed inthe annual mean northward winds in the years 1993-2006. Based on these observations, an extensive study hasbeen carried out to understand the long-term behaviour of the MLT winds over tropics. The results obtained willbe presented and discussed during the meeting.

SA32-2

DELTA Campaign: Coordinated Rocket and Ground-based ObservationsJunichi Kurihara1, Shin-ichiro Oyama1, Satonori Nozawa1, Ryoichi Fujii1, Yasunobu Ogawa2, Naomoto Iwagami3, and Takumi Abe4

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Cikusa-ku, Nagoya 464-8601, Japan2. National Institute of Polar Research, Research Organization of Information and Systems, Itabashi-ku, Tokyo 173-8515,Japan3. Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033,Japan4. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 229-8510,Japan

In order to investigate the dynamics and energetics in the polar lower thermosphere, coordinated sounding rocketobservation with ground-based Fabry-Perot Interferometers (FPIs) and the European Incoherent Scatter (EISCAT)radar was successfully conducted during the Dynamics and Energetics of the Lower Thermosphere in Aurora(DELTA) campaign on 13 December 2004. The neutral temperature measured by the rocket-borne instrument is70 - 140 K higher than the MSIS model above 110 km but is consistent with the FPI observations. The EISCATobservation suggests the presence of a strong Joule heating at 110-130 km altitudes from 30 minutes before to 1hour after the rocket launch and this event coincides with strong vertical winds observed by the FPI.Based on these results from the DELTA campaign in 2004, the DELTA-2 campaign is planned in January 2009.In the next campaign, the field of view of the EISCAT radar and FPIs will be overlapped with the rocket trajectoryto directly compare observed parameters. In addition, the rocket will release Trimethyl Aluminum (TMA) alongthe trajectory and neutral wind measurement will be made simultaneously with neutral temperature measurement.

- 37 -

SA32-3

Equinox Transition of the Mesospheric Temperature Field - RevisitedMarianna G. Shepherd1, Young-Min Cho1, Gordon G. Shepherd1, Christoph Jacobi2, Werner Singer3, Dirk Offermann4, Michael Bittner5, Marty Mlynczak6, and Jonathan H. Jiang7

1. Centre for Research in Earth and Space Science, York University, 4700 Keele St. Toronto, ON, M3J 1P3, Canada2. Institute for Meteorology, University of Leipzig, Stephanstr, 3, 04103 Leipzig, Germany3. Leibniz-Institute of Atmospheric Physics, Schloss-Srt. 6, Kuhlungsborn, D-18225, Germany4. Bergische Universitat-GH Wuppertal-Fachbereich Phyisik, Wuppertal, Germany5. German Aerospace Center (DLR), German Remote Sensing Data Center, Oberpfaffenhofen, D-82234 Wessling, Germany6. NASA Langley Research Center, Hampton, Virginia, USA7. Jet Propulsion Laboratory, Mail Stop 183-701, 4800 Oak Grove Drive, Pasadena, California 91109, USA

Airglow emission and temperature observations by the WINDII/UARS experiment and ground-based stationsrevealed a rapid rise in the nighttime emission rate in spring time followed by a subsequent decrease in themagnitude, which was termed the 'springtime transition'. A rapid temperature enhancement was also revealed inthe average annual temperature at 87 km height in observations from 1991 to 1998. Large amplitude perturbationsin mesospheric Na-lidar and OH rotational temperatures at 87 km around autumnal equinox were also reportedboth at middle and high Northern latitudes. The seasonal temperature variation of the middle and high latitudeMLT region is determined by the global vertical/meridional circulation and a meridional circulation from thesummer to the winter polar regions. The dynamical structure of the MLT region is also perturbed on a long-periodtime scale of days to approximately a month by planetary waves, but also by rapid wind field changes e.g. owingto stratospheric warmings. All these temperature studies employed observations only at 87 km from the 1990s,when no major stratospheric warmings were observed in the Northern hemisphere. In this report the response ofthe MLT temperature field is examined during periods of major stratospheric warmings, from December 2003 toMay 2006, employing ground-based rotational temperatures from OH and O2 airglow observations at 87 km and94 km, temperature data from the SABER/TIMED and MLS/AURA experiments and meteor radar wind andtemperatures.

SA32-4

Vertical Motions in the Upper Mesosphere and Lower Thermosphere in theContext of the Large-scale CirculationGordon G. Shepherd1, Young-Min Cho1, and Guiping Liu2

1. Centre for Research in Earth and Space Science, York University, Toronto, Canada M3J 1P32. Meteorological Service of Canada, Environment Canada, 4705 Dufferin Street, Toronto, Canada

Observations with WINDII on the NASA UARS spacecraft show large vertical motions of the oxygen airglow,with a total range of about 7 km, at all latitudes viewed. Ground-based measurements of airglow emission ratesand molecular rotational temperatures from Resolute Bay, 74 N, in Northern Canada show a strong correlation ofemission rate and temperature for short-term perturbations as well as variations over the course of a winter, andeven from winter to winter. Studies have been carried out to relate these observations to the WINDIImeasurements, including the global pattern of airglow emission, and its variation with altitude, local time andseason. An annual pattern is found of emission rates that are high during winter, and low during summer thatparallels the mesospheric temperatures that are also high in winter and low in summer; that same as found atResolute Bay. Superimposed on this pattern is a brief emission rate peak during mid-summer. This pattern extendsupwards through the hydroxyl layer, but at the higher altitude of the O(1S) emission the pattern changes. At thesealtitudes the pattern becomes semi-annual, with maxima at equinoxes, indicating that the strong meridional flowof the large-scale circulation does not extend to these altitudes. In addition, the mesospheric perturbationscorrelate with those in the lower stratosphere indicating strong vertical coupling. These results are described anddiscussed.

- 38 -

SA41I-1

Sensitivity of the MLT to the Lorenz Energy Cycle of the TroposphereErich Becker

Institute of Atmospheric Physics, Germany

The mesosphere and lower thermosphere (MLT) is modulated by solar variability and dynamically controlledfrom below. In order to separate the two influences on a longer time scale it is necessary to fully assess thedynamical control.Conventional climate models cannot fully describe the sensitivity of the MLT to changes in the troposphere. Thereason is that this sensitivity is largely controlled by the generation, propagation, and dissipation of gravity waves(GWs), and that GWs are conventionally parameterized by assuming a fixed GW source at a single level in thetroposphere. Since the Eliassen-Palm flux (EPF) of low-frequency inertia GWs tends to vanish, the maincontribution to the EPF divergence at high latitudes of the MLT is due to mid- and high-frequency GWs withperiods of a few hours or less. In order to resolve at least a good portion of these waves in a GCM, a high spatialresolution from the boundary layer to the lower thermosphere is required. Furthermore, both the generation anddissipation of resolved GWs strongly depends on the details of the parameterization of turbulence. In the present study we propose a new formulation of a mechanistic GCM with high spatial resolution and asophisticated parameterization of turbulence. This model explicitly simulates the wave drag of the MLT thatresults from self-consistent GW sources in the troposphere. The Smagorinsky-type horizontal and verticaldiffusion coefficients are scaled by the Richardson criterion such that no sponge layer is required for the GWs todissipate in the MLT. Sensitivity experiments show that an intensification of the Lorenz energy cycle, as may beassociated with climate change, leads to the following effects in the summer MLT: downshift of the residualcirculation, as well as stronger dissipation, lower temperatures, and reduced easterlies below the mesopause.These changes are consistent with enhanced tropospheric GW sources, leading to GW dissipation at loweraltitudes in the summer MLT. The same signature of changes in the MLT was observed during NH summer 2002.

SA41I-2

Upward Propagation of Atmospheric Waves and Its Impact on the GeneralCirculation in the ThermosphereYasunobu Miyoshi1 and Hitoshi Fujiwara2

1. Dept. Earth and Planetary Sciences, Kyushu University, Hakozaki, Fukuoka, 812-8581, Japan2. Dept. Geophysics, Tohoku University, Aobaku, Sendai, 980-8578, Japan

Upward propagating atmospheric waves play an important role on the general circulation in the thermosphere. Byusing a general circulation model (GCM) that contains the region from the ground surface to the upperthermosphere [Miyoshi and Fujiwara, 2003], dynamical coupling processes between the lower and upperatmosphere by atmospheric waves have been investigated. In this study, we examine day-to-day variations ofplanetary scale waves (such as Rossby wave and tides) in the lower thermosphere and their relations with thelower atmosphere. Our results show that day-to-day variations of planetary scale waves are evident in the lowerthermosphere, and are closely related with the atmospheric variation in the lower atmosphere. Furthermore, ahigher horizontal resolution GCM (horizontal resolution: 140km) is used to investigate upward propagation ofsmaller scale waves. In the lower thermosphere, fluctuation associated upward propagating gravity waves isclearly seen. Fluctuation associated with upward propagating gravity waves above 150 km height is alsodiscussed.

- 39 -

SA41I-3

Advanced Meteor Radar Observation with the MU Radar for ObservingTridimensional Structure of Horizontal Velocities and Cooperative OpticalObservationsTakuji Nakamura1, Masaki Tsutsumi2, Takuya D. Kawahara3, and Kazuo Shiokawa4

1. Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Kyoto 611-0011, Japan2. National Institute of Polar Research, Tokyo, Japan3. Faculty of Engineering, Shinshu Univ., Nagano, Japan4. STE laboratory, Nagoya Univ., Toyokawa, Aichi, Japan

The MU radar meteor echo observation with 1 MW transmission power has been used to derive precise horizontalwind velocities in the MLT region (80 - 100 km). A new receiving system with a 29 digital quadrature detectionwas attached to the MU radar in 2004. We have applied the new MU radar system for meteor echo observation.Coherently integrated 25 channel receiving signals improved the SNR of meteor echoes significantly, and meteorecho number became as large as 50,000 per a day, which is about five times of previous meteor observations withthe MU radar. The high-rate meteor echoes were utilized to detect horizontal distribution of wind velocity field ofabout 50 km scale. The limited area for determining wind velocity significantly changed the characteristics ofwind velocity variation within the field of view (FOV) of 300 - 400 km, and enabled to detect wind perturbationsdue to horizontally propagating waves such as gravity waves. The comparison with the airglow imaging hasshown that similar wave structures were observed both the radar and the imager, suggesting capability ofsimultaneous observation of an identical wave. A sodium temperature lidar is also operated in order to deriveatmospheric stability of the background of the wave propagation. External receiving systems for measuringforward scatter of meteor echoes are being built, which also will contribute to clarification of detailedhorizontal/vertical structure of MLT region.

SA41I-4

On the Seasonal and Interannual Variability of the Migrating Diurnal TideDavid A. Ortland

NorthWest Research Associates

The amplitude of the migrating diurnal tide in the mesosphere and lower thermosphere varies seasonally and isalso significantly correlated with the quasi-biennial oscillation (QBO) within the stratosphere. It is likely that thetide amplitude is modulated by a combination of mechanisms, including variable heating and gravity waveinteraction. However, in 2002 Charles McLandress showed that variability of the mean winds through which thetides propagate can reproduce a significant portion of the observed tide variability. This talk will presentmechanistic model simulations that further explore this mechanism for tidal variability and which show how tideamplitude seasonal and QBO variations are controlled directly by the structure of the zonal mean background nearthe stratopause. Model tide amplitudes calculated using tropospheric heating alone have only minor variabilitydue to seasonal changes in the heating and mean wind structures. Significant tide amplitude variations arereproduced only when the ozone tidal heating is also included in the model. Ozone heating occurs over a broadaltitude range, and this causes the tide response to be quite sensitive to changes in the zonal mean backgroundstructure within the heating region. This will be explained in terms of the vertical structure equation forgeneralized Hough modes. The modulated tide response to ozone heating can alternate between constructive anddestructive interference with the tide response to troposphere heating, producing significant amplitude modulationof the combined response in the MLT.

- 40 -

SA41I-5

The Aeronomy of Ice in the Mesosphere MissionScott M. Bailey1 and James M. Russell2

1. 302 Whittemore Hall Virginia Tech Blacksburg, VA 24061, USA2. Center for Atmospheric Sciences Hampton University Hampton VA 23668, USA

The Aeronomy of Ice in the Mesosphere (AIM) satellite was launched on April 25, 2007. The overall goal of theAIM mission is to resolve why Polar Mesospheric Clouds (PMCs) form and why they vary. By measuring PMCsand the thermal, chemical and dynamical environment in which they form, AIM will quantify the connectionbetween these clouds and the meteorology of the polar mesosphere. This will provide the basis for the study oflong term variability in the mesospheric climate and its relationship to global change. The results of AIM will be a rigorous validation of predictive models that can reliably use past PMC changes andpresent trends as indicators of global change. This goal will be achieved by measuring PMC abundances, spatialdistribution, particle size distributions, gravity wave activity, cosmic dust influx to the atmosphere and precise,vertical profile measurements of temperature, H2O, OH, CH4, O3, CO2, NO, and aerosols. The AIM satellitecarries three instruments including the Solar Occultation for Ice Experiment (SOFIE), the Cloud Imaging andParticle Size Experiment (CIPS) and the Cosmic Dust Experiment (CDE). This talk will summarize the sciencegoals, measurement requirements, the expected performance of the AIM instruments and any early resultsavailable at the time of the symposium.

SA41-1

Wind Balance in the Mesosphere and Lower ThermosphereHan-Li Liu1, Daniel R. Marsh2, Qian Wu1, and Jiyao Xu3

1. High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO 80307-3000, USA2. Atmospheric Chemistry Division, National Center for Atmospheric Research, Boulder, CO 80307-3000, USA3. State Key Laboratory for Space Weather, Chinese Academy of Sciences, Beijing 100080, China

The wind balance in the mesosphere and lower thermosphere is revisited in this study. Using simulation resultsfrom the Whole Atmosphere Community Climate Model (WACCM), it is demonstrated geostrophic balance is nolonger valid in the zonal direction due to the large zonal gravity wave foricng. As a result, the zonal mean geostrophic meridional wind is significantly different from the actual zonal meanmeridional wind, and the residual mean merdional circulation derived from geostrophic winds is much weakerthan that derived from model winds.It is also shown that the ageostrophic contribution comes primarily from gravity wave forcing, so that there is anapproximate three-way balance between pressure gradient, Coriolis force, and gravity wave forcing.The relationship between the geostrophic winds and actual winds is also tested using measurements from TIMEDSABER and TIDI instruments.

- 41 -

SA41-2

Observations of Polar Mesosphere Summer Echoes with Calibrated VHFRadars at 69 Degree in the Northern and Southern Hemisphere:Interhemispheric SimilarityRalph Latteck1, Werner Singer1, Ray J. Morris2, Damian J. Murphy2, and David A. Holdsworth2

1. Leibniz-Institut fuer Atmosphaerenphysik, Kuehlungsborn, Germany2. Australian Antarctic Division, Kingston, Tasmania, Australia

Polar Mesosphere Summer Echoes (PMSE) have been observed with 50-MHz VHF radars in the NorthernHemisphere for more than 20 years. However measurements in the Southern Hemisphere were in the past rare andlimited to low southern latitudes. In 2003 the Australian Antarctic Division installed a 55-MHz VHFradar atDavis, Antarctica (68.6 degree S), located at a comparable southern geographical latitude to Andenes, Norway(69.3 degree N), where the Leibniz-Institute of Atmospheric Physics operates a 50-MHz radar for more than 10years.PMSE observed in the northern and southern hemisphere were studied using continuous measurements obtainedby absolute calibrated VHF radars located at Andenes and Davis. The PMSE observed at Davis have a lower peakvolume reflectivity of approximately 4*10^(-11) 1/m compared with their counterparts (7*10^(-10) 1/m) observedat Andenes. The duration of the PMSE season is highly correlated with the dynamical and thermal state of themesopause re-gion as shown by simultaneously measured meridional winds and temperatures. PMSE occurredless frequently but with greater variability above Davis. The diurnal variation of PMSE occurrence has amaximum around 11-16 LT in both hemispheres, and a minimum occurs during late evening with a longerduration in the southern hemisphere. The mean PMSE sea-son at both sites started around 34 days before solstice,but the duration of the Davis PMSE season is about 10 days shorter than in the northern hemisphere at theequivalent latitude. The mean peak altitude of the PMSE extent at Davis is about 1km higher than the mean peakaltitude of 85 km known from northern hemispheric observations at Andenes.

- 42 -

SA42I-1

Gravity Wave Breaking and Instability at High Reynolds Numbers:Implications for Energy Transfers, Momentum Fluxes, Measurement Biases,and Other SurprisesDave Fritts, Tom Lund, Kam Wan, Ling Wang, and Joe Werne

NWRA/Colorado Research Associates, Boulder CO

Gravity waves (GWs) exhibit a wide range of instabilities that span all GW amplitudes and intrinsic frequencies.Linear theory provides a useful guide to initial instability structures and growth rates, but no guidance for theimpacts on primary GW amplitudes. Numerical studies indicate a competition between 2D and 3D dynamicsacross the amplitude spectrum, while superposed low-frequency GWs or oscillatory mean motions dramaticallyaccelerate energy transfers. Turbulence accompanying breaking is strongly correlated with the GW phase, but isalso highly variable in intensity and highly anisotropic throughout the evolution. Results exhibit correlations thatindicate a potential for significant measurement biases, and which appear to account for a number of radarobservations to date. As turbulence subsides, a quasi-2D motion field evolves having a layered thermal andvelocity structure similar in some respects to that arising from turbulence due to KH instability.

SA42I-2

Development of a T213L256 Middle Atmosphere General Circulation ModelShingo Watanabe1, Yoshio Kawatani1, Yoshihiro Tomikawa2, Masaaki Takahashi3, and Kaoru Sato4

1. Frontier Research Center for Global Change, Japan Marine Science and Technology, Showa-machi 3173-25, Kanazawa-ku,Yokohama city, 236-0001, Japan2. National Institute of Polar Reserch, 9-10, Kaga 1-chome,Itabashi-ku, Tokyo 173-8515, Japan3. Center for Climate System Research, University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa-shi, Chiba, 277-8568, Japan4. Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku,Tokyo 113-0033 Japan

We have developed a high-resolution middle atmosphere general circulation model (AGCM) for studyingatmospheric gravity waves and their effects on large-scale fields. The AGCM has T213 spectral truncation in thehorizontal and 256 layers in the vertical from the surface to about 85 km (i.e., vertical spacing of 300 m). Whilethe T213 horizontal resolution is still not sufficient to resolve small scale gravity waves (i.e. minimum horizontalwavelength is about 188 km), the vertical resolution is high enough to resolve large part of gravity waves whichare observed. The high vertical resolution is important for studying gravity waves, because gravity wavescontinuously change their properties in the course of vertical propagation. It is also important for studyingwave-wave interaction among waves with different vertical wavelengths. Gravity waves are spontaneouslygenerated by convection, topography, and instability in the AGCM. No gravity wave drag parameterization isused in the AGCM. The AGCM is being integrated for 3 years. In this talk, some basic results are compared tothose observed, i.e., the zonal mean zonal winds and temperature, static stability, and wave spectra. Reality ofpossible source mechanisms for gravity waves is briefly discussed. In order to investigate relative importance ofplanetary waves, large-scale gravity waves, and small scale gravity waves for maintaining large-scale zonal windstructures in the middle atmosphere, Eliassen-Palm diagnostics are separately applied for the three groups ofwaves with different horizontal wavelengths.

- 43 -

SA42I-3

Toward the Global Atlas of Middle-Atmospheric Gravity WavesDong L. Wu

Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA

Determining global gravity wave (GW) morphology from the troposphere to thermosphere is essential forimproving numerical climate and weather models. With rapid advances in satellite observations and mesoscalemodeling, it is feasible now to diagnose the model skills directly with satellite data for global gravity wavegeneration and propagation. Because GWs have a broad range of horizontal and vertical wavelengths, satelliteobservations can be used to constrain the morphology of certain portions of the wave spectra. To bridgeobservation and model efforts in GW research, we studied temperature perturbations in the latest ECMWF(European Center for Medium range Weather Forecasting) T799L91 analyses, and compared the ECMWF GWvariances with satellite observations at altitudes up to ~60 km.

SA42I-4

Utilizing Airglow Measurements to Investigate Short-Period Gravity WaveCoupling at Mesospheric HeightsMichael J. Taylor, Mitsumu K. Ejiri, and Yucheng Zhao

Center for Atmospheric and Space Sciences, Utah State University, Logan, UT 84322-4405, USA

It is now widely accepted that the deposition of momentum by small-scale, freely propagating gravity waves playsa key, systematic role in defining the global-scale circulation, as well as, regional dynamical variability atmesospheric heights. Excited primarily by strong convection, topography, and wind shears in the loweratmosphere, these waves propagate upwards and are filtered by the variable wind field as they transport energyand momentum into the upper atmosphere. The subsequent deposition of gravity wave momentum flux withinthis region arises from wave instability and dissipation processes. Long-term, passive optical observations of thecoupling of these waves into the mesosphere and lower thermosphere (MLT) region (~80-100 km) are facilitatedby several naturally occurring, vertically distinct nightglow layers. This talk focuses on airglow measurementsfrom a number of sites, using a range of imaging instrumentation, and summarizes recent investigations of wavepropagation and event momentum flux estimates, providing new results of wave coupling and dissipation effects.

- 44 -

SA42I-5

Wintertime Temperature Maximum at the Subtropical Stratopause in aT213L256 AGCMY.Tomikawa1, S.Watanabe3, Y.Kawatani3, K.Miyazaki3, M.Takahashi3, and K. Sato2

1. National Institute of Polar Research, Tokyo 173-8515, Japan2. The University of Tokyo, Tokyo 113-0033, Japan3. Frontier Research Center for Global Change, Kanagawa 236-0001, Japan4. CCSR/Univ. of Tokyo

Temperature and zonal wind structures around the tropical and subtropical stratopause region have been studiedusing the Center for Climate System Research/National Institute for Environmental Studies/Frontier ResearchCenter for Global Change (CCSR/NIES/FRCGC) AGCM. The AGCM has T213 spectral truncation in thehorizontal and 256 layers in the vertical from the surface up to 85 km (i.e., vertical spacing of 300 m). Gravitywaves are spontaneously generated by convection, topography, instability, and any adjustment processes in theAGCM with no gravity wave drag parameterizations. The AGCM successfully reproduces a quasi-biennialoscillation (QBO)-like oscillation with a period of about 15 months in the tropical stratosphere. The semiannualoscillation (SAO) reproduced in the AGCM has an easterly maximum during the solstice in the lower mesosphereof the summer hemisphere subtropics. An interesting feature is that a temperature maximum appears at thesubtropical stratopause in the winter hemisphere, simultaneously with the easterly maximum of the stratosphericSAO in the summer hemisphere. In fact, a careful looking at the CIRA-86 climatology shows that the wintertimetemperature maximum at the subtropical stratopause is clearly evident. The transformed Eulerian-mean (TEM)analysis demonstrates that the temperature maximum is induced by strong downwelling of meridional circulationpassing above the tropical stratopause where the absolute angular momentum contours are nearly horizontal.Easterly phase of the stratospheric SAO reduces the absolute angular momentum above the tropical stratopause,and makes a corridor permitting a strong meridional circulation along the nearly-horizontal contours of absoluteangular momentum across the equator. On the other hand, the westerly phase of SAO acts as a barrier forcross-equatorial meridional circulation, in which the absolute angular momentum contours are almost vertical.This feature implies that there is preferred height and season for cross-equatorial tracer transport owing to thephase of SAO. It would have a large impact on tracer concentration and tracer age in the upper stratosphere andmesosphere.

- 45 -

SA42-1

Acceleration of the Brewer Dobson Circulation due to Increases inGreeenhouse GasesRolando R. Garcia

National Center for Atmospheric Research, Boulder, CO, USA

Recent work with climate models indicates that the age of stratospheric air becomes younger and the BrewerDobson Circulation (BDC) accelerates as greenhouse gases increase. The result appears to be robust, being foundin most model reconstructions of the climate of the 20th century and in prognostic simulations of the 21st century. We examine calculations made with the Whole Atmosphere Community Climate Model (WACCM) covering theperiod 1950-2050 to investigate the mechanisms responsible for these changes. In WACCM, the acceleration ofthe BDC is driven by enhanced divergence of EP flux in the subtropical lower stratosphere up to about 25 km;above this altitude, changes in momentum deposition by parameterized gravity waves accelerate the BDC in themiddle and upper stratosphere. These changes are significant in the Tropics, subtropics, and midlatitudes, butthere is no statistically significant change of the circulation at subpolar or polar latitudes; in particular, there is nosignificant change in the frequency of sudden warmings or of temperature in the wintertime polar stratosphere. Itis shown that changes in the BDC explain concurrent changes in age of air and affect the pattern of predictedozone recovery in the 21st century.

SA42-2

Impact of Energetic Particle Precipitation on High-Altitude Nitric AcidEnhancements : 6 Years of Observations with the ODIN SatelliteYvan J. Orsolini1, Joachim Urban2, and Donal Murtagh2

1. Norwegian Institute for Air Research (NILU), Kjeller, Norway2. Chalmers University of Technology, Goteborg, Sweden

We investigate the impact of energetic particle precipitation on the chemistry of the middle atmosphere, and focusin particular on the high-altitude enhancements in nitric acid in the polar upper stratosphere in winter, in bothhemispheres. Nitric acid is a key minor constituent with a multi-facetted role in the stratospheric ozone chemistry.These stratospheric polar enhancements are seen recurrently but display a considerable inter-annual variability.They have been linked to fluxes of NOx generated by energetic particle precipitation, either coming down fromthe mesosphere or in-situ in the stratosphere. The strong enhancements in NOx and nitric acid, and theaccompanying ozone decrease, in the aftermath of the exceptional solar storms of the autumn 2003 have been welldocumented, with the availability of global observations from several instruments (e.g. MIPAS, GOMOS, ODIN,?c). Through slow descent within the polar vortex, chemical perturbations propagate down into the lowerstratosphere.We examine observations of high-altitude nitric acid enhancements by the ODIN satellite over the years2001-2007. We demonstrate that they often follow a two-stage development, and we examine the factorsgoverning their formation, and in particular the role of energetic particle precipitation, and its interplay withstratospheric dynamical perturbations (e.g. SSWs) and rapid mesospheric descent.

- 46 -

SA51I-1

A Lagrangian Spectral Parameterization of Convective Gravity WavesHye-Yeong Chun1, Hyun-Joo Choi1, and In-Sun Song2

1. Department of Atmospheric Sciences, Yonsei University, Seoul, 120-749, Korea2. Global Modeling and Assimilation Office, NASA/GSFC, USA

A Lagrangian spectral parameterization of gravity wave drag (GWD) induced by cumulus convection isdeveloped and implemented into the NCAR Whole Atmosphere Community Climate Model (WACCM). Basedon ray theory, the Lagrangian parameterization explicitly calculates gravity wave (GW) propagation that has beentreated too simply in column-based parameterizations. For direct comparison with column-based parameterization,a hydrostatic and Boussinesq version of the Lagrangian parameterization is used in the present study. GW packettrajectories demonstrate that the Lagrangian parameterization calculates reasonably the GW-packet propagationand that the horizontal extent of GW propagation can be as large as 20 degree as GWs approach their criticallevels. Comparison with column-based parameterization through one-month simulations indicates that the overallstructures of GWDC are similar to one another, but the magnitude is much increased in the lower stratosphere andequatorial troposphere in the model with the Lagrangian parameterization. This magnitude difference is duemainly to the vertical convergence of GW packets. In climate simulations, it is found that the zonal-mean zonalwind in the equatorial stratosphere and along the axis of the polar night jet is improved through the Lagrangianparameterization. Also, interannual variability in the equatorial lower stratosphere is significantly enhanced. Theparameterization is validated by off-line calculations using TRMM and ECMWF data, and resultant temperaturevariance is compared with those observed in satellites. It is found that the Lagrangian parameterization producesmore realistic distribution of gravity waves than that by the currently used column-based parameterization.

SA51I-2

Coupling of Atmospheric Tides with the Lower BoundaryKevin Hamilton

Meteorology/IPRC, University of Hawaii, Honolulu, Hawaii 96822, USA

The vertically propagating components of the atmospheric tides are effectively global-scale inertia-gravity wavesthat are forced mainly by solar heating. Classical tidal theory and many more sophisticated numerical treatmentshave ignored the interaction between the tide and topography at the lower boundary. In the real world,observations of the surface tidal pressure variations (S(p)) display some some quite large and systematic regionaland local variability that has not been explained in detail, but must involve interactions with topography. This talkwill consider how the atmospheric tides couple with topography and how this can explain some prominent aspectsof the observations of tides at the surface. Also the earlier speculation of Fels (1977) that the momentum andenergy exchanges between tides and the solid earth are important for the global tide will be reexamined.

- 47 -

SA51-1

Middle Atmosphere Disturbance during 1998 - 2004 Winter Seasons in theWestern ArcticKazuyo Sakanoi1, Yasuhiro Murayama2, Richard L. Collins3, and Kohei Mizutani2

1. Komazawa University2. National Institute of Information and Communications Technology3. Geophysical Institute, University of Alaska, Fairbanks

Observations of mesospheric temperature and wind by a Rayleigh lidar and MF radar at Poker Flat ResearchRange (PFRR: 65.1N, 147.5W), Chatanika, Alaska are conducted by NICT (National institute of Information andCommunications Technology, Japan) and the Geophysical Institute, the University of Alaska, Fairbanks (USA).We present characteristics of disturbance of the winter middle atmosphere in the western Arctic using the NICTRayleigh lidar and MF radar data, and stratospheric assimilation data provided by the United KingdomMeteorological Office on a period that extends from November 1998 to April 2004.Seven major SSWs occurred during analyzed period except for 2002/2003 winter season. Horizontal wind reversal(Eastward to Westward) and temperature disturbance (increase/decrease/no stratopause etc.) were often observedmainly associated with SSWs: temperature increasing of 10 - 30 K in the lower mesosphere and intermittentreversals of East-West wind were observed before major SSWs, disappear of temperature peak as stratopause andtemperature was almost constant from 40 - 80 km altitude range just before major SSWs, temperature decreasingof 10 - 20 K in the lower mesosphere and East-West wind reversal (eastward to westward) from 30 - 90 kmaltitude range during major SSWs. The wind reversal started and descended from mesosphere to upperstratosphere and occasionally to troposphere.In addition, remarkable elevation of the stratopause (from 55km to 70km) and the center altitude of middleatmosphere jet occurred after a major SSW in 2003/2004 winter season.

SA51-2

3-D Activities of Equatorial Gravity Waves in a High-resolution AGCMYoshio Kawatani1, Masaaki Takahashi2, Shingo Watanabe1, Saburo Miyahara3, and Kaoru Sato4

1. JAMSTEC/Frontier Research Center for Global Change, Yokohama, 236-0001, Japan2. Center for Climate System Research, University of Tokyo, Kashiwa, 277-8568, Japan3. Department of Earth and Planetary Science, University of Tokyo, Tokyo, 113-0033, Japan4. Department of Earth and Planets, Kyushu University, Fukuoka, 812-8581, Japan

Due to relatively small temporal and spatial scales of GWs, Atmospheric General Circulation Model (AGCM) isone of the effective tools to study GWs globally (cf. Sato et al. 1999; Kawatani et al. 2003, 2004, 2005; Watanabeet al. 2006). CCSR/NIES/FRCGC AGCM with resolution of T213L256 is used in the present study. The verticalresolution is set about 300 m with top boundary of ~80km. Although no gravity wave drag parameterization isincluded in the model, the QBO-like oscillation is clearly simulated. The amplitude of easterly (westerly) phase is~30m/s (20m/s) with bottom levels around 80 hPa. Recently, Miyahara (2006) derived a three dimensional wave activity flux applicable to inertio-GWs. The fluxgives the wave-action density flux relative to the local time mean flow. Results using this flux show that in theequatorial upper troposphere, convectively generated GWs which large vertical flux of eastward (westward)momentum is associated with are excited in the Eastern (Western) Hemisphere. The Walker circulation which hasdifferent direction of zonal wind between the Eastern and Western Hemisphere plays crucial roles on selectivefiltering of GWs. Spectrum analysis reveals that in the upper troposphere and lower stratosphere strong eastward(westward) forcing due to GWs is formed over easterly (westerly) of the Walker circulation. In the altitude wherethe phase of QBO changes from easterly to westerly, eastward forcing in the Eastern Hemisphere is much greaterthan that in the Western Hemisphere. 3-D distribution of equatorial waves and its roles on QBO will be alsodiscussed.

- 48 -

SA51-3

General Characteristics of Gravity Waves in the Troposphere and LowerStratosphere during Convection over Indonesia and IndiaS.K. Dhaka1, Y. Shibagaki2, M. K. Yamamoto3, H. Hashiguchi3, S. Fukao3, and H.-Y.Chun4

1. Department of Physics, Rajdhani College, University of Delhi, Delhi, India2. Osaka Electro-Communication University, Japan3. Research Institute for Sustainable Humanosphere, Kyoto University, Japan4. Department of Atmospheric Science, Yonsei University, Seoul, South Korea

In the past, a few campaigns were conducted to observe gravity waves associated with convective systems atGadanki (13.5 N, 79.2 E) using Indian MST radar. Most recently two special CPEA campaigns with broadobjectives were organized during April - May 2004 and Nov- Dec 2005 using several instruments, which werewell coordinated with the main Equatorial Atmosphere Radar (EAR) at Koto Tabang (0.2S, 100.3 E). We haveinvestigated general characteristics of convection-induced gravity waves at both the locations. During convectiveevents radar reflectivity showed the temporal evolution of convection with different intensities and shapes overradar site. In some cases, convection noted quickly growing and penetrating in to upper troposphere within fewtens of minute. On the other hand, there were cases when convection was not intense and its growth was verygradual in the troposphere. Interestingly, differences in vertical velocities are also noted at these two locations; atGadanki (Indian radar site) it is noted up to 10 m/s, where as at Koto Tabang (EAR site) velocity is lesser by afactor of two to three. Common feature of short vertical wavelength (lambda_z ~ 2-4 km) occurrence in verticalwind in the upper troposphere and lower stratosphere (UTLS), noted at both the locations during convectionsuggesting short short vertical wavelength as one of the preferential scale of forcing of convection-inducedgravity waves. Dynamics in UTLS region seems largely affected by the interaction of gravity waves with shortlambda_z to the background wind.

SA51-4

High-resolution Observations of the Temporal and Spatial Variability ofGravity Wave Potential Energy Using COSMIC Satellite DataSimon P. Alexander and Toshitaka Tsuda

Research Institute for Sustainable Humanosphere (RISH), Kyoto University, Gokasho, Uji 611-0011 JAPAN

The six COSMIC (Constellation Observing System for Meteorology, Ionosphere & Climate) satellites werelaunched in mid-2006 and are providing several thousand global profiles of temperature and water vapour per daybelow 40km. This high-resolution dataset can be used to examine coupling processes between the stratosphere andtroposphere. The temperature data were used to obtain tropospheric and stratospheric gravity wave potentialenergy (PE). The temporal variability of gravity wave emissions from three sources: convection, topography andjet-stream activity were investigated. Regional COSMIC data from Indonesia, Antarctica and Japan were used todetermine the variability and relation with background wind conditions obtained from model data.Results from the first year of COSMIC operation will be presented, showing strong seasonal, annual andlocational variations in gravity wave activity. Tropical results over the Indonesian region showed modulation ofUTLS PE by the MJO, and stratospheric wave filtering by the QBO. Equatorial longitudinal PE variability will bediscussed. Enhancements in stratospheric PE above Japan during winter are compared with the Eliassen-Palm fluxand the mid-latitude winter jet. Initial results from the Antarctic region will also be presented.

- 49 -

SA52I-1

Attribution of Decadal Variability in Lower-Stratospheric Tropical OzoneDaniel R. Marsh and Rolando R. Garcia

National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307-3000, USA

The variability of ozone in the lower stratosphere in a climate-chemistry modelis investigated by multipleregression nalysis. The model includes forcing due to changes in solar irradiance and to anomalies in sea surfacetemperatures (SST). When ozone calculated for the period 1979-2003 is regressed against time and 10.7 cm radioflux (f10.7), the regression coefficient of f10.7 at 52 hPa is 2.8% per 100 units. This decreases to 1.8% if alagged index of El Nino-Southern Oscillation (ENSO) is included in the regression, and to 0.78% if the period ofanalysis is extended to 1950-2003. The last value is in good agreement with simulations of fixed solar maximum vs. solar minimum conditions thatdo not include SST variability. These results suggest that some of the decadal variability in tropical ozonepreviously attributed to solar variability may instead be related to the occurrence of ENSO events.

SA52I-2

Stratosphere-Troposphere Coupling and Climate ChangeMark Baldwin

Northwest Research Associates, USA

The paradigm of a separate stratosphere and troposphere is advantageous when describing quantities such ashumidity, ozone, lapse rate, and potential vorticity. However, the continuous atmosphere allows vertical wavepropagation, exchange of mass, and other interactions between these layers. In many respects the distinctionbetween the stratosphere and troposphere is artificial. The dynamical coupling of the stratosphere and troposphereis primarily mediated by waves that propagate upwards, into the stratosphere, where they dissipate causingvariability of the stratospheric flow.The conventional view is that of a one-way interaction in which tropospheric waves drive stratospheric variability.This view has given way to a more sophisticated understanding of a two-way interaction Observations and modelstudies show that the stratosphere organizes chaotic wave forcing from below to create long-lived charges to thestratospheric circulation. These stratospheric changes can feed back to affect weather and climate in thetroposphere. Similarly, charges to the stratospheric circulation from changes in solar radiation, radiatively activetrace gases, or other causes can also affect tropospheric weather and climate.There are three primary areas in which stratosphere-troposphere coupling is important: 1) extended-range weatherforecasts, 2) climate predictions, and 3) predictions of the evolution and recovery of the ozone layer. In this talk, Iwill provide an overview of stratosphere-troposphere coupling and discuss aspects of these three topics.

- 50 -

SA52-1

Simulating the Changes of the NAO during Pre-industrial Time and in aFuture Climate Scenario with a Fully CoupledStratosphere-Troposphere-Ocean ModelUlrich Cubasch, Thomas Spangehl, and Ulrike Langematz

Meteorological Institute, Free University Berlin, Carl-Heirich-Becker-Weg 6-10, 12165 Berlin, Germany

The role of natural and anthropogenic forcing on the climate in the North-Atlantic is investigated using thecoupled stratosphere-troposphere-ocean model. This model consists of a combination of the atmosphere modelECHAM4 with an extension to the middle atmosphere (T30/L39) and the ocean model HOPE-G.To simulate the pre-industrial climate, the solar forcing, the forcing by volcanic aerosols and the greenhouse gasconcentration are prescribed. For the future climate, ensemble simulations using the SRES scenario A2 have beencarried out.During the Maunder Minimum (1645-1715) and during the Dalton Minimum (1790-1830) the model simulates asignificant global cooling. The cooling is particularly strong north of Iceland, and in the North-Atlantic betweenNewfoundland and the southern tip of Greenland. In these regions this temperature change is connected to anincrease of sea ice. The NAO, however, is hardly changing during the pre-industrial period. The present dayclimate, however, shows a shift of the NAO-index towards positive values and a general increase in troposphericwesterlies in mid-latitudes. In a future climate an increase in the frequency of stratospheric winter warmings can be seen. This perturbs thestratospheric polar vortex which in turn affects tropospheric variability, which is confirmed by a comparison withthe simulations without explicit representation of the stratosphere. The inclusion of the stratosphere leads to aweaker increase of the tropospheric westerlies in mid-latitudes and a less pronounced shift of the NAO towardsmore positive values. The synoptic systems move less towards the North than in the simulations withoutstratosphere.

SA52-2

Radar and Optical Observations at Adelaide, AustraliaIain M Reid1, David A Holdsworth2, Daniel McIntosh1, Robert A Vincent1, Jonathan Woithe2, and Abas Sivjee3

1. School of Chemistry and Physics, University of Adelaide, Adelaide, Australia2. ATRAD Pty Ltd, Thebarton, South Australia, Australia3. Embry-Riddle Aeronautical University, Daytona Beach, FL, USA

This paper presents comparisons of nightglow, MF radar and VHF radar meteor observations using instrumentsinstalled at Buckland Park (34.9S, 138.6E), Australia. The Buckland Park MF radar has operated continuouslysince 1984. The Buckland Park ST radar was installed in 2004, primarily for observation of stratospheric andtropospheric echoes, but with external transmit and receive antennas installed to allow all-sky interferometricmeteor radar observations. The Adelaide meteor radar was installed in 2003 to allow all-sky interferometricmeteor radar observations. A 558 nm photometer has operated continuously at the site since 1995, and an O2 andOH spectrometer since 2001. The intensity of the OI 558 nm nightglow emission exhibits spring and autumn enhancements, bright nights andclear seasonal and interannual periodicities. It also exhibits a solar cycle dependence. Like many othermid-latitude observations, the autumn enhancement is greater than the spring enhancement. A Lomb periodogramanalysis of the intensity indicates the presence of annual, semi-annual and quasi-biennial oscillations. Theobservations are consistent with Adelaide being a transitional latitude between a dominant semi-annual oscillationobserved at low latitudes and the dominant annual oscillation observed at mid-latitudes. Recently however,Shepherd et al. (2006) have argued for a more complex relationship between latitudinal variations in intensitybecause of sampling effects of some instruments and tidal variations throughout the year, and this is discussed inthe context of our observations.

- 51 -

SA52-3

Determining Mesospheric Temperatures from Meteor Radar Observationsat King Sejong Station (62 deg S, 58 deg W), AntarcticaYong Ha Kim1, Jeong-Han Kim1, Chang Sup Lee2, and Geon Hwa Jee2

1. Dept. of Astronomy and Space Science, Chungnam National University, Daejeon 305-764, Korea2. Korea Polar Research Institute, Incheon 406-840, Korea

A VHF meteor radar has been installed in March 2007 at King Sejong Station(62 deg S, 58 deg W), Antarctica. The meteor radar can measure numerous meteor trails, and their decay rates provide ambipolar diffusioncoefficients at meteor altitudes, 70 - 110 km. The diffusion coefficient is known to be closely connected to thelocal atmospheric temperature and density. In this study, we investigate the relations between the ambipolardiffusion coefficients and rotational temperatures of O2(0-1) and OH(6-2) airglows simultaneously measured by aspectral airglow temperature imager (SATI). Correlation coefficients of the relations are derived for variousaltitudes ranging from 80 to 100 km. The altitudes that have maximum correlation coefficients may beconsidered as altitudes of the airglow layers. The derived relations will be used to estimate mesospherictemperatures at other altitudes. The estimate mesospheric temperatures will be compared with satelliteobservations. Seasonal variations in the maximum correlation altitudes will also be compared with works in otherlatitudes.

SA52-4

Current Status of Program of the Antarctic Syowa MST/IS RadarKaoru Sato1, Masaki Tsutsumi2, Toru Sato3, Akinori Saito4, Yoshihiro Tomikawa2, Koji Nishimura2, Takashi Yamanouchi2, Takehiko Aso2, and Masaki Ejiri2

1. Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan2. National Institute of Polar Research, Tokyo 113-0033, Japan3. Department of Communications and Computer Engineering, Kyoto University, Kyoto 606-8501, Japan4. Department Geophysics, Kyoto University, Kyoto, 606-8502, Japan

PANSY is a plan to introduce the first MST (Mesosphere-Stratosphere-Troposphere) /IS (Incoherent Scatter)radar, which is a VHF monostatic pulse Doppler radar, in the Antarctic to Syowa Station (39E, 69S) as animportant station observing the earth's environment with the aim to catch the climate change signals that theAntarctic atmosphere shows. This radar consists of about 1000 crossed Yagi antennas having a power of 500kWwhich allows us to observe the Antarctic atmosphere in the height region of 1-500 km. The interaction of theneutral atmosphere with the ionosphere and magnetosphere as well as the global-scale atmospheric circulationincluding the low and middle latitude regions are also targets of PANSY. The observation data with highresolution and good accuracy obtained by the PANSY radar are also valuable from the viewpoint of certificationof the reality of phenomena simulated by high-resolution numerical models. After a series of feasibility studies conducted in the last several years, a small pilot radar system is to be installedat Syowa Station during the austral summer of 2007/2008 in order to test newly developed power-efficienttransmitters and light-weight antennas and will start observing the polar mesopause region as a meteor wind radaras an activity of IPY2007-2008 (a part of ICESTAR/IHY). Numerical and observational works of atmosphericwaves related to this project will be also presented.

- 52 -

SB11I-1

Enhanced Heating near the Footpoints of Coronal Loops in Solar ActiveRegionsHirohisa Hara1 and Louise K. Harra2

1. National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, JAPAN2. Mullard Space Science Laboratory, University College London, Holmbury, St Mary, Dorking, Surrey, RH5, 6NT, UK

The Hinode EUV Imaging Spectrometer has observed the upflow and enhanced nonthermal velocities near thefootpoints of solar active region loops from a spectroscopic observation in the extreme-ultraviolet ranges. Weshow that the upflow speed is subsonic and that the enhanced nonthermal velocities decrease exponentially frombottom toward the apex of coronal loops. Implication of our ovservation for the heating of coronal loops isdiscussed.

SB11I-2

An Investigation into the Initiation Mechanism of a Solar Flare Based on theObserved Nature of Photospheric Magnetic FieldTetsuya Magara1, Takaaki Yokoyama2, Satoshi Inoue3, Kiyoshi Ichimoto1, Yukio Katsukawa1, Shin'ichi Nagata4, and Saku Tsuneta1

1. National Astronomical Observatory of Japan2. Tokyo University3. Nagoya University4. Kyoto University

The solar photosphere is a special place where a lot of observational information on plasma motions and magneticfields is available. The photospheric activity shown by solar plasma presents a key to understanding themechanism for energetic phenomena such as flares observed in the solar atmosphere. These phenomena couldgive a significant impact on the solar-terrestrial environment. In this talk we focus on how the photosphericactivity relates to the initiation of a flare using fine-scale observations provided by Hinode. The analysis ofobserved data demonstrates that the photospheric evolution of an active region (NOAA 10930) takes severaldistinct phases toward causing a flare. We show the detailed nature of each of these phases and discuss how theactive region accumulates free magnetic energy that is used to cause the flare.

- 53 -

SB11-1

Hinode SOT-XRT Observations of Solar Microflares: Magnetic Fields andChromospheric Signatures at the Footpoints of Loop-type TransientBrigteningsToshifumi Shimizu1, Ryohei Kano2, Yukio Katsukawa2, Masahito Kubo3, Edward DeLuca4, Kiyoshi Ichimoto2, Bruce Lites3, Shin'ichi Nagata5, Taro Sakao1, Richard Shine6, Yoshinori Suematsu2, Theodore Tarbell6, Alan Title6, and Saku Tsuneta2

1. ISAS/JAXA, Sagamihara, Kanagawa 229-8510, Japan2. NAOJ, Mitaka, Tokyo 181-8588, Japan3. HAO/NCAR, Boulder, CO 80307, USA4. SAO, Cambridge, MA 02138, USA5. Kyoto University, Takayama, Gifu 506-1314, Japan6. LMSAL, Palo Alto, CA 94304, USA

Solar active regions have been known to produce numerous numbers of small-scale explosive energy releases, i.e.,microflares, which energy scale is much smaller than normal flares. They are observed with imaging observationsin soft X-rays as transient brightenings of small-scale coronal loops. They are morphologically full of variety;point-like brightenings with diameter less than 10 arcsec. brightenings of a single short loop-like structure, andsimultaneous brightenings of multiple number of coronal loops. Owing to its higher spatial resolution, HinodeX-Ray Telescope (XRT) is revealing finer soft X-ray structures involved in brightenings, giving temporaldevelopment on spatial distribution of heated coronal plasma in coronal magnetic fields. Solar microflares areobservationally important not only for understanding their contribution in generating higher temperaturecomponent of coronal plasma but also for understanding the fundamental physics of transient energy releases inthe solar atmosphere. Solar microflares may be a proto-type energy release compared with major complicatedflares. In investigations on the physics of transient energy releases, it is expected to give some key observationalclues by exploring magnetic activities and magnetic field configuration at the footpoints of brightening loops withsimultaneous visible-light observations by Hinode Solar Optical Telescope (SOT). This study is focusing onmagnetic field configuration and its activities observed at the footpoints of multiple-loop brightenings, which havebeen extremely lack of photospheric magnetic field observations in high spatial resolution. For our investigationsof corona-photosphere magnetic coupling, we have established co-alignment between SOT and XRT withaccuracy better than 1 arcsec (Shimizu et al. PASJ submitted). Then we are investigating how the chromosphericsignatures can be observed at the footpoints of brightening loops (CaIIH) and what kind of characteristics are seenin magnetic-field data (G-band, Magnetogram, Stokes Polarimter data). In some of multiple-loop beightenings,two small ribbons are simultaneously observed in CaII H images, which should contain the footpoints of transientbrightening loops. One of the ribbons are located well inside the sunspot unmbra. This paper will report onchromospheric signatures and the magnetic field configuration of solar microflares observed with Hinode.

- 54 -

SB11-2

Detection of Coronal Alfven Waves in a Solar Prominence with the HinodeSolar Optical TelescopeTakenori J. Okamoto1, Saku Tsuneta1, Thomas E. Berger3, Kiyoshi Ichimoto1, Yukio Katsukawa1, Bruce W. Lites4, Shin'ichi Nagata2, Kazunari Shibata2, Toshifumi Shimizu5, Richard A. Shine3, Yoshinori Suematsu1, Theodore D. Tarbell3, and Alan M. Title3

1. National Astronomical Observatory, Mitaka, Tokyo, 181-8588, Japan2. Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto, 607-8471, Japan3. Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover St., Palo Alto, CA 94304, USA4. High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder CO 80307-3000, USA5. ISAS/JAXA, Sagamihara, Kanagawa, 229-8510, Japan

Solar prominences are cool 10,000 K plasma clouds supported in the surrounding 1,000,000 K coronal plasma byas-yet-undetermined mechanisms. They are the most enigmatic of solar structures, often serving as the source of``coronal mass ejections'', large-scale eruptions of plasma from flaring solar active regions, that can have majorimpacts on the terrestrial magnetic environment. The new Japanese solar physics satellite Hinode recently carriedout observations of a large active region prominence seen near the solar limb. Hinode enables the highestresolution images of prominences yet seen, with a temporal uniformity that allows multi-hour diffraction-limited``movies'' to be constructed, a feat that is impossible in ground-based observations.The new prominence movies from Hinode show fine-scale thread-like structures with widths of at most 150 kmoscillating in the plane of the sky with periods of several minutes. Analysis of the oscillations suggests that theyare Alfven waves propagating along magnetic field lines in the prominence. This represents the first directdetection of Alfven waves propagating on coronal magnetic field lines and establishes Hinode as an importantnew tool for the study of magnetohydrodynamic physics in the coronae of Sun-like stars.

SB11-3

Ubiquitous Sporadic Horizontal Magnetic Fields on the Photosphere withHINODE/SOTRyohko Ishikawa1, Saku Tsuneta2, Hiroaki Isobe1, Kiyoshi Ichimoto2, Yukio Katsukawa2, Bruce W. Lites3, Shin'ichi Nagata4, Toshifumi Shimizu5, Richard A. Shine6, Yoshinori Suematsu2, Theodore D. Tarbell6, and Alan M. Title6

1. University of Tokyo, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan2. National Astronomical Observatory, Mitaka, Tokyo, 181-8588, Japan3. High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder CO 80307-3000, USA4. Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto, 607-8471, Japan5. ISAS/JAXA, Sagamihara, Kanagawa, 229-8510, Japan6. Lockheed Martin Solar and Astrophysics Laboratory, B/252, 3251 Hanover St., Palo Alto, CA 94304, USA

The Sun has intense magnetic fields with various time and special scales on its surface. These magnetic fieldsemerge from the interior, and their precise measurement is crucial for the understating of global and local dynamoprocess inside the Sun, coronal and chromospheric heating and flares. We discover a new form of emergingmagnetic fields with the solar optical telescope aboard Hinode. A plage region produces small-scale, ubiquitous,and transient horizontal magnetic fields. The field strength is around or sometimes exceeds the equi-partition fieldfor local convective flow, and the diameter of the horizontal flux tubes is much smaller than the size of granules.The spectro-polarimetric data clearly shows that these horizontal magnetic fields are tossed about by upflows anddownflows of convection. The horizontal fields appear with preferred direction, which is consistent with theplage-region's global fields. The coherent directivity and ubiquity of the horizontal fields indicate the underneathextended reservoirs of horizontal fields presumably provided by a global dynamo. A local dynamo process mayact on such horizontal fields to have stronger fields. Comparing the frequency, the directivity and the magneticfield configuration of these horizontal magnetic fields in the plage, quiet sun, and coronal hole regions, we willclarify nature of the transient horizontal fields and discuss its implication to solar dynamo.

- 55 -

SB11-4

Hinode SOT/SP Observations of a Magnetic Structure of a Dark Filamenton the SunT. Yokoyama1, Y. Katsukawa2, M. Shimojo2, S. Tsuneta2, Y. Suematsu2, K. Ichimoto2, T. Shimizu3, S. Nagata4, M. Kubo5, B. W. Lites5, H. Socas-Navarro5, and Hinode Japan/US SOT team

1. Dept, Earth and Planetary Sci., U. Tokyo, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan2. NAOJ, Mitaka, Tokyo, 181-8858, Japan3. ISAS, JAXA, Sagamihara, Kanagawa, 229-8510, Japan4. Hida Obs., Kyoto U., Takayama, Gifu, 506-1314, Japan5. HAO, NCAR, Boulder, CO80307-3000, U.S.A.

The structure of the photospheric vector magnetic field beneath a dark filament on the Sun is studied by using theHinode SOT/SP observations. The magnetic structure of a solar dark filament is an interesting subject since it isrelated with the dynamics during its eruption. Such eruption is frequently associated with a flare and a CME thatis a source of the disturbance on the terrestrial magnetosphere. There are two models suggested. One is the modelin which the filament material is on top of the bended arcade field lines. In the other model, a flux rope structure isassumed. This type of structure has an 'inverse-polarity' orientation beneath the filament, namely the orientation ofthe tangential magnetic field on the surface is from the negative to the positive vertical magnetic poles. Theproposed theoretical models on the eruption assume a structure including a flux rope. Lites (2005) studied thephotospheric magnetic field beneath a filament and found that its magnetic structure is consistent with a flux rope.But the number of such observations is still limited and more samples are necessary. By using the Hinode SOT/SPdata, we studied a filamentin active region NOAA 10930. Hinode SOT/SP enables us to obtain a high spatial andhigh accuracy vector magnetic maps on the photospherebeneath this filament. The investigated part of thefilament sits almost along a constant latitude, namely in the east-west direction along a magnetic neutral line. Thenorthern side has negative vertical magnetic components. The tangential field has a direction almost parallel to thefilament with a slight shear with an azimuth angle of 160 degree defined from the western orientation. This angle,however, contains an ambiguity in the orientation due to the 180-degree ambiguity in the Stokes fitting procedure. In order to know its orientation, i.e.if it is in the normal orientation or in the inverse one, we need to solve thisambiguity. We used the limb observations for the solution.When the filament is near the east limb, we found thatthe line-of-site magnetic component beneath is positive, while it is negative near the west limb. This change ofsign indicates that the axial field along the filament is in the western orientation. By putting together these, weconclude that the filament has an 'inverse-polarity' magnetic structure, namely a flux-rope structure.

- 56 -

SB11-5

Particle Acceleration and Magnetic Field Configuration in Arcade-TypeSolar FlaresSatoshi Masuda and Satoshi Inoue

Solar-Terrestrial Environment Laboratory, Nagoya University

Hard X-ray emissions from footpoints of flare loops show precipitation of accelerated electrons. In arcade-typeflares, a lot of flare loops in soft X-rays and two-ribbon structure in H-alpha along the arcade. However, in hardX-rays, usually clear two-ribbon structure is not observed except one event (the 14-July-2000 flare). Does thismean electron acceleration takes place only in some special magnetic loop among many loops which formed anarcade? One possibility is that electron acceleration takes place everywhere in the whole arcade system, butdynamic range of hard X-ray imaging instruments is too small to detect all of hard X-ray emissions. Thissituation might happen if electron acceleration efficiency strongly depends upon the local magnetic field strengthwhich varies enormously along an arcade system. In this paper, we investigated the relationship between hardX-ray intensity and magnetic field strength along the arcade system by using Yohkoh/HXT and SoHO/MDI data. Assuming some magnetic connectivity between the two ribbons, we found a weak correlation between them.

SB11-6

Discovery of Chromospheric Anemone Jets with Hinode/SOTKazunari Shibata1, Tahei Nakamura1, Takuma Matsumoto1, Kenichi Otsuji1, Takenori J. Okamoto1, Naoto Nishizuka1, Tomoko Kawate1, Hiroko Watanabe1, Shin'ichi Nagata1, Satoru Ueno1, Reizaburo Kiatai1, Satoshi Nozawa3, Masaki Shimizu1, Hinode J team2, and Hinode U team5

1. Kwasan and Hida Observatories, Kyoto University2. National Astronomical Observatories3. JAXA/ISAS4. Ibaraki University5. Lockheed Martin Solar and Astrophysics Laboratory6. High Altitude Observatory

A new Japanese solar mission, Hinode, is revealing an amazingly new views of the Sun that even the lower solaratmosphere, hromosphere, is highly dynamic and is full of tiny jets and nanoflares. Here we report the discoveryof chromospheric ``anemone jets'' outside of sunspots in active regions with the Solar Optical Telescope aboardHinode. The typical length and width of the jets are 3'' - 7'' = 2000 - 5000 km and 0.2'' - 0.4'' = 150 - 300 km,respectively, and their velocity is 10 - 20 km s^-1. Probably, these are the smallest solar jets observed so far. Thestriking feature of these jets is their morphology: their shape looks like an inverted Y-shape, similar to the shapeof X-ray ``anemone-jets'' in the corona, suggesting that the reconnection similar to that in the corona is occurringin much smaller spatial scale in the chromosphere. This further suggests the new concept of ubiquitousreconnection in the solar atmosphere, as a key for solving the long-standing puzzle of the coronal heatingmechanism.

- 57 -

SB12I-1

Ubiquitous Jet-Like Activities in Sunspot ChromospheresYukio Katsukawa1, Saku Tsuneta1, Yoshinori Suematsu1, Kiyoshi Ichimoto1, Toshifumi Shimizu2, Shin'ichi Nagata3, Thomas E. Berger4, Theodore D. Tarbell4, Richard A. Shine4, and Alan M. Title4

1. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan2. Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan3. Kwasan and Hida Observatory, Kyoto University, Yamashina, Kyoto 607-8471, Japan4. Lockheed Martin Solar and Astrophysical Lab, 3251, Hanover St., Palo Alto, California 94304, USA

We discovered fine-scale jet-like activities, called penumbral micro-jets, in chromospheres of sunspot penumbraewith the Solar Optical Telescope (SOT) on the new Japanese solar physics satellite HINODE. They are ubiquitousactivities in the penumbral chromosphere, and can be seen frequently and everywhere in Ca II H movies ofsunspots taken with SOT. Not only their small spatial scale of 400 km but their short duration less than 1 minutemake it difficult to identify them in existing observations. The micro-jets are possibly caused by magneticreconnection in complex magnetic configuration in penumbrae, and have a potential to heat the corona above asunspot.

SB12I-2

Observations of the Early Phases of Prominence EruptionsHiroaki Isobe1, Durgesh Tripathi2, Cristina Chifor2, Helen E. Mason2, Ayumi Asai3, and Rekha Jain4

1. Department of Earth and Planetary Science, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan2. Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Wilberforce Road, Cambridge CB30WA, UK3. Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamisaku, Nagano 384-1305, Japan4. Department of Applied Mathematics, University of Sheffield, Hicks building, Hounsfield Road, Sheffield S3 7RH, UK

Solar flares, coronal mass ejections and prominence eruptions are most likely the different aspects of a singlephenomenon that involves plasma ejection and magnetic reconnection. The mechanisms of the eruption,particularly its trigger, are of great importance from the view point of the space weather. Prominence eruptionevents provide the best oppotunity to study the trigger of solar eruptions, because prominences clearly visualizethe magnetic structure of the erupting flux systems, or at least a part of them. In this paper we present two kinds ofobservations of the early phases of prominence eruptions. One is a large-amplitude oscillation of an eruptingprominence. A clear oscillatory motion was found in a prominence while it was slowly rising toward fast eruption.Such slow-rise motion are quite common in solar eruptions. The oscillation is clear evidence that during the slowrise the prominence retains an equilibrium, and hence the slow rise is a quasi-static motion rather than a linearstage of an instability. The other is a multi-wavelength observation of a prominence eruption on the solar limb.We found a X-ray precursor simultaneous with the onset of slow rise of the prominence. During the slow rise, theprominence underwent a weak and then strong heating, as seen in microwave and EUV. This indicates magneticreconnection of field lines connected to the prominence itself. We will discuss the possible implication of theseobservations for the trigger and three-dimensional dynamics of solar eruptions.

- 58 -

SB12I-3

Solar Chromospheric Dynamics and HeatingMats Carlsson

Non-radiative energy input is required to maintain the million degree Solar corona. This coronal heating problemhas remained unexplained for more than 50 years. It is sometimes forgotten that the layer between the photosphereand corona, the solar chromosphere, contains a thousand times as much mass as the corona and requires 25-50times more energy for its heating. In addition, the energy required for the coronal heating and the acceleration ofthe solar wind may have its origin in the chromosphere or below. One reason for the lack of focus on thechromosphere is that it is difficult to observe and the physical regime goes from domination by the plasma todomination by the magnetic fields. Our understanding of this fascinating region of the solar atmosphere hasadvanced significantly with the event of new observing facilities and advances in numerical modelling.This talk will highlight recent observations of the chromosphere from the Swedish solar telescope on La Palmaand from the Hinode satellite and interpretations through 3D MHD modelling.

SB12-1

Full Sun Temperature Diagnostics with Hinode X-ray TelescopeNoriyuki Narukage1, Masumi Shimojo2, Taro Sakao1, Ryohei Kano3, Saku Tsuneta3, Kiyoto Shibasaki2, Edward E. DeLuca4, Mark A. Weber4, Steven H. Saar4, and Patricia R. Jibben4

1. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara, Kanagawa229-8510, Japan2. Nobeyama Solar Radio Observatory, National Astronomical Observatory of Japan, Nobeyama, Nagano, 384-1305, Japan3. National Astronomical Observatory of Japan, Mitaka, Tokyo, 181-8588, Japan4. Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, United States

The sun has various and dynamic features based on the coronal observations in X-rays, which can not be imaginedfrom the sun seen with our naked eye. The solar corona has wide temperature range from less than 1MK to morethan 10MK. The X-ray telescope (XRT) on board Hinode satellite has 9 X-ray analysis filters with differenttemperature responses to detect such various coronal plasma. Using the data observed with this telescope, wesuccessfully derived the coronal temperature around the whole sun. And we found that coronal structures arenicely classified using the temperature and emission measure. To considering the heating balance, this means thatthe coronal structures are determined with the length of structure and heating flux. This might be the great clue tosolving the big question of the coronal heating why the hot 1MK corona is stably exist above the cool 6,000Ksolar surface. Furthermore, the full sun temperature distribution is useful for the space weather as the initialcondition of the simulation.

- 59 -

SB12-2

Medium-Scale Traveling Ionospheric Disturbances Detected withHigh-Resolution TEC Maps over North AmericaTakuya Tsugawa1, Anthea Coster2, Yuichi Otsuka1, and Akinori Saito3

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Japan2. Massachusetts Institute of Technology Haystack Observatory, USA3. Graduate School of Science, Kyoto University, Japan

New characteristics of medium-scale traveling ionospheric disturbances (MSTIDs) are detected withhigh-resolution detrended TEC maps over North America. The detrended TEC data are obtained by subtracting a60-minute running average from the original TEC data at each ionospheric penetration point (IPP). TEC data arecollected from multiple GPS networks in North America. Currently detrended TEC data from 1,400 GPS receivers(as of December 2006) and at all IPPs are mapped onto the thin shell ionosphere at 300 km altitude, where thedata is binned and averaged. The detrended TEC maps cover a wide area of 70-130 deg W and 28-48 deg N, andhave a spatial resolution of 1x1 deg in latitude and longitude, and a temporal resolution of 30 seconds.A preliminary examination of these TEC maps from January through December 2006 reveals several newcharacteristics of MSTIDs, including:1. Nighttime MSTIDs propagating southwestward with 200-500 km wavelengths are frequently observed overNorth America in summer and winter similarly to those observed over Japan. It is revealed that their wavefrontcan be extended longer than about 2,000 km and has already been long since their appearance.2. Daytime equatorward MSTIDs with 300-1000 km wavelengths are frequently observed in winter. The daytimeMSTIDs propagate southeastward prior to noon while the MSTIDs post-noon propagate southwestward. TheseMSTIDs are superimposed on each other around the post-noon period.Although coordinated observations with other observation techniques, such as incoherent scatter (ISRs) radars andall-sky airglow imagers, are needed to clarify the generation and propagation mechanism of these MSTIDs, thedetrended TEC maps over North America are a powerful tool to investigate space weather phenomena.

SB12-3

Comparison Study of Different Mass Emission Lines on Active RegionShinsuke Imada1, Hirohisa Hara1, Tetsuya Watanabe1, Ayumi Asai2, Suguru Kamio1, and Keiichi Matsuzaki3

1. National Astoronomical Observatory of Japan2. Nobeyama Solar Radio Observatory3. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency

Understanding of coronal heating is one of the major targets of Hinode mission. One of the plausible mechanismsfor coronal heating is interaction with MHD waves. Within this category, one of the most important parameter forheating is mass / charge. In this presentation, we present the comparison study of different mass emission lines onthe active region. We compare between Iron emission lines and Silicon/Sulfur emission lines. Iron andSilicon/Sulfur emission lines cover various corona temperature (from logT = 5.8 to 6.6). The mass ratio betweenIron and Silicon/Sulfur is roughly two. We discuss the effect of mass difference to coronal characteristics by usingline ratio, Doppler shift, and line width.

- 60 -

SB12-4

The Properties of the Ca II/G-band Bright Points around the PenumbraMasumi Shimojo1, Saku Tsuneta1, Yoshinori Suematsu1, Kiyoshi Ichimoto1, Yukio Katsukawa1, Toshifumi Shimizu, Shin'ichi Nagata3, and Hinode SOT/XRT Team

1. NAOJ2. ISAS/JAXA3. Kyoto-U

Due to the very high spatial resolution and the continuous observation of SOT/Hinode, we found that the Ca IIbright points penetrated to the west edge of the penumbra of the NOAA10923 preceding spot on 15 November,2006. The velocity of the penetrated bright points is ~0.6 km/s and is similar to the transverse velocity of the supergranule. It suggests that the moat region does not exist in the early phase of the sunspot. Two days after, the brightpoint still penetrated to the edge of the penumbra. But, we found that a part of MMFs expands to outer of thepenumbra. After one rotation, the sunspot definitely showed the moat region at the west edge of the penumbra.The observation shows that the moat region is forming while interacting between the sunspot, the super granulesand the network magnetic field. It is very important thing for understanding of the decay of the sunspot. In orderto study the interaction, we investigate the motion and magnetic field of bright points using SOT-FG, SOT-SP andXRT data. At result, we found following facts: 1) The penetrated Ca II bright has the counter bright points inG-band image. 2) The Ca II/G-band bright points disappear during moving to the penumbra edge. 3) The magneticfield strength of the penetrated bright points is about 1300 gauss. And the magnetic field is vertical, is not similarto that of penumbra. 4) Between the edge of penumbra and the network magnetic field, there are relatively brightX-ray loops. From the results, we discuss the relationship between the sunspot decaying, the super granule and thenetwork magnetic field.

SB12-5

Temperature Structures above Coronal Hole Boundary and Quiet SunR. Kano1, T. Sakao2, N. Narukage2, J. Kotoku1, T. Bando1, E. DeLuca3, L. Lundquist3, and XRT Team

1. National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan2. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency,Sagamihara, Kanagawa 229-8510,Japan3. Harvard-Smithsonian, Center for Astrophysics, Cambridge, MA 02138, U.S.A.

We present vertical temperature structures above the quiet Sun derived with the off-limb observations of the X-rayTelescope (XRT) aboard Hinode. Because X-ray intensity above the limb is fainter than that of disk corona, it isimportant to estimate the scattered light from the disk corona. For such estimation, we used the XRT data duringthe solar eclipses on February 17 and March 19 in 2007 at the Hinode orbit, and derived the coronal temperaturewith the filter-ratio method. On February 17, the Moon occulted a southern polar coronal hole and radial structures rooted at the coronal holebooundary. The temperature along the radial structures increases from the footpoints (1.9 - 2.1 MK) to the heightof about 100Mm (2.2 - 2.3MK), and then keeps almost constant value until 200Mm. On March 19, the Moonocculted the quiet Sun near the nourth-east limb. In XRT images, only diffuse corona is seen above the limb. Thetemperature of the diffuse corona is 2.0 - 2.1MK at the base and decreases with height gradually.Two temperature structures are completely different each other. The difference is probably because of thedifference of magnetic configuretion: In the former case, magnetic fields run vertical, but in the latter case, thecorona is filled with many closed loop magnetic fields. We also present the coronal hole temperature and density observed during the solar eclipse on February 17, anddisscuss their relationship with the solar wind.

- 61 -

SB21I-1

Plasma Flows in the Solar Corona and their Implications to the Solar WindTaro Sakao1, Ryouhei Kano2, Noriyuki Narukage1, Jun'ichi Kotoku2, Takamasa Bando2, Edward E. DeLuca3, Patricia R. Jibben3, and Saku Tsuneta2

1. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 229-8510,Japan2. National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan3. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA

We present soft X-ray imaging observations with the X-Ray Telescope (XRT) aboard Hinode, with emphasis onplasma flows in the corona. The XRT has revealed, in the active region NOAA AR 10942 observed in February2007, continuous outflow of plasmas along apparently-open magnetic field lines emanating from one end of a pairof bi-polar magnetic structure that constitutes the active region, adjacent to a coronal hole. Projected velocity ofthe outflowing plasmas ranges, say, from 100 to 170 km/s, with its typical value ~140 km/s. Filter-ratio analysis with multiple filters of the XRT provides temperature of ~1.4 MK and density ~2 x 10^9/cm^3 for the source region of the outflowing plasmas. Assuming that the entire fraction of the outflowingplasmas were to escape to the interplanetary space along the open field lines, this would then lead to a total massloss rate of ~2 x 10^11 g/s, which reaches to a good fraction of the mass loss rate estimated for the solar wind. Even apart from this observation, the XRT provides ample examples of clear patterns of continuous outflows fromboundaries of coronal holes, and along field lines rooted inside coronal holes. XRT observations of such plasma flows in the corona are reviewed and their possible implications to the solarwind discussed.

SB21I-2

Convections in Sunspots Observed by SOT/HinodeKiyoshi Ichimoto1, Richard A. Shine2, Bruce W. Lites3, Masahito Kubo3, Toshifumi Shimizu4, Yoshinori Suematsu1, Saku Tsuneta1, Yukio Katsukawa1, Theodore D. Tarbell2, Alan M. Title2, Shin'Ichi Nagata5, Takaaki Yokoyama6, Masumi Shimojo1, Thomas Berger2, and Takashi Sekii1

1. National Astronomical Observatory of Japan2. Lockheed Martin Advanced Technology Center3. High Altitude Observatory, National Center for Atmospheric Research4. Japan Aerospace Exploration Agency, Institute of Space and Astronoutical Science5. Kwasan and Hida Observatory, Kyoto University6. University of Tokyo

The sunspots, which form the solar active regions producing vital phenomena in outer solar atmosphere, are lowtemperature regions on the solar surface. Their coolness is explained by the suppression of the photosphericconvective motions due to the strong magnetic fields. The sunspots are not completely dark however. The umbraeand penumbrae have a brightness of about 10% and 70% of the normal solar atmosphere, respectively, and acertain amount of energy still needs to be supplied to maintain their brightness. Since there is no definiteobservational evidence of efficient convections in sunspots, the brightness of the sunspot is one of the unsolvedproblems in solar physics.Thanks to its excellent spatial resolution, the Solar Optical Telescope (SOT) abord Hinode reveals small scaledynamic motions in sunspots. If we call the phenomena in which relatively hotter gas moves upward and coolergas moves downward as 'convection', the SOT/Hinode discovered the candidates of several types of convections; 1) Up flow and down flows in both ends of the Evershed flow, 2) 'Twisting' motions of penumbral filaments,3) Motions in umbral dots, 4) Convection-like motions in and around light bridge.

- 62 -

The 'twisting' motions of the penumbral filaments are found only when the penumbral filament is observedobliquely from a side, and are thought to be a manifestation of the convective motion rather than actual turn of thepenumbral filaments. We present the observational evidences showing these new features, and make initial attempt of the quantitativeevaluation of energy flux in sunspots especially with a special attention on those in the penumbrae.

SB21-1

A New View of Space Weather - Combining IPS and STEREO HIObservations of the Solar Wind with Studies of Ionospheric ConsequencesAndy Breen1, Chris Davis2, Gareth Dorrian1, Richard Fallows1, Huw Morgan4, Mario Bisi3, Helen Middleton1, Emma Whittick1, Danielle Bewsher2, Richard Harrison2, Steve Crothers2, Jackie Davis2, Chris Eyles5, Peter Thomasson6, and Gudmund Wannberg7

1. University of Wales Aberystwyth, Penglais Hill, Aberystwyth, Ceredigion SY23 3BZ, Wales2. Rutherford-Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, England3. University of California San Diego, 9500 Gilman Dr., La Jolla, California CA 92093, U.S.A.4. University of Hawai'i, 2680 Woodlawn Drive, Honolulu, Hawai'i HI 96822, U.S.A.5. University of Birmingham, Edgbaston, Birmingham, B15 2TT, England6. Jodrell Bank Observatory, University of Manchester, Jodrell Bank, Macclesfield, Cheshire SK11 9DL, England7. EISCAT Scientific Association, P.O. Box 164, SE-981 23 Kiruna, Sweden

The availability of data from the Heliospheric Imager instruments on the STEREO spacecraft provide the firstdetailed view the Sun-Earth line. Such observations reveal structure and movement of large-scale features, and areperfectly complemented by ground-based radio scintillation (IPS) measurements of speed and direction ofsmall-scale structure.In this paper we present results from a co-ordinated programme of measurements bringing together STEREO HI,IPS and ionospheric tomography.We combine STEREO HI observations of structures in solar wind with IPS measurements of solar wind speedfrom EISCAT and MERLIN, while ionospheric tomography data and modelling are used to study the response ofthe Earth's ionosphere to solar wind variations. We discuss the observations and our methodology, before goingon to draw conclusions for the events observed and discuss the lessons learned for future observing campaigns.

- 63 -

SB21-2

Impacts of a Torus Model on Determining Geometries of Magnetic CloudsKatsuhide Marubashi and Cho Kyung-Suk

Korea Astronomy and Space Science Institute, Yuseong-Gu, Daejeon, 305-348, Korea

Magnetic clouds (MCs) can occupy the whole body or a significant part of ICMEs. Determining their magneticstructures and geometries is of fundamental importance to examine the relationships between MCs and thecausative solar phenomena. Structures of MCs have been analyzed by using cylindrical flux rope models in mostof the foregoing studies. However, if we accept a global configuration of MC, a huge loop extending from theSun, it is obvious that we need another model to describe the magnetic field variations observed when thespacecraft passed the flank of the loop. Some curvature effects must be taken into account in the model. Here weanalyze MCs using a torus-shaped flux rope model as a possible way to approximate the local structure of the MCloop near its curved flank part. It should be noted that we are not saying that the whole MC be torus-shaped. First,we show that the torus model yields the features of magnetic field variations which cannot be reproduced bycylinder models. They include cases of magnetic field rotations through large angles substantially larger than 180degrees, and cases in which magnetic field vectors rotate mainly in the X-Y plane. Then, we show the analysisresults obtained by applying the torus model to some representative observed MCs. It is seen that the torus modelfitting yields the geometrical relationships between the magnetic fields in MCs and the solar magnetic fieldswhich are more acceptable than cylinder models.

SB21-3

Parametric Instabilities of Finite Amplitude Alfven Waves in the Solar WindYasuhiro Nariyuki and Tohru Hada

E.S.S.T., Kyushu U., Japan

Large amplitude, low-frequency Alfven waves constitute one of the essential and ubiquitous elements in the solarwind. These waves may be regarded as "robust" fluctuations in space plasma, as they can propagate long distancebefore they are eventually dissipated by various collisionless damping processes. This is an important point inexamining the heating and acceleration of the solar corona and the solar wind, since the loading of momentum,energy, and helicity conveyed by the Alfven waves is completed when the waves damp away. It is believed thatparametric instabilities are one of the most reliable processes in dissipation of such Alfven waves. In this talk, wewill report recent progress of parametric instabilities of Alfven waves.Parametric instabilities of Alfven waves with cold ion (i.e. MHD and/or Hall-MHD systems) are vastly differentfrom those in a finite ion beta plasma, even when the collisionless damping of the Alfven waves are neglected.Further, parametric instabilities of "non-monochromatic (incoherent)" Alfven waves are also qualitativelydifferent from those of "monochromatic (coherent)" waves due to the nonlinearly driven instabilities. We will alsodiscuss possible parameterization of the various dissipation effects of the Alfven waves.

- 64 -

SB21-4

Origin of Disappearing Solar Wind EventsKen'ichi Fujiki1, Taichi Murakami1, Masayoshi Kojima1, Munetoshi Tokumaru1, Hiroaki Ito1, and P. K. Manoharan2

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, 464-8601,Japan2. Radio Astronomy centre, NCRA-TIFR, Ooty, India

An extremely low-density solar wind event, "the disappearing solar wind event", of May 11-12, 1999, has beenanalyzed in detail using solar wind speed and density measurements from different data bases. It is inferred thatthis event has been caused by the abnormally low-speed flow originating above a small-sized coronal hole. Inorder to understand the solar origin of speed and density of such extreme events, we identified 22 events of lowdensity and speed events from the Advanced Composition Explorer (ACE) data. These data sets exclude periodsof CME transients. The following results have obtained: (1) a clear indication that the extreme events are causedby mid-latitude coronal holes; (2) correlation between the drop in density below the ambient value and theduration of the event; (3) associated changes in the magnetic field components; (4) in particular, changes in speedcomponents and their correlation with the magnetic field components; (5) the prevailing anti-correlation betweenthe Vy and density. Nearly 50% of the extreme events can be explained by dominant correlation between thespeed in the y-direction and density.

SB21-5

Three-Dimensional Structure of the Solar Wind Near the SunMasaaki Amano, Takayuki Umeda, and Tatsuki Ogino

Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan

Geospace environment changes have become an important problem because troubles of the satellite may seriouslyaffect human daily life. It often connects with magnetic storms which are originated by Interplanetary disturbanceejected from the sun.It is well known from Parker model that the solar wind becomes supersonic beyond a critical radius. Thetwo-dimensional structure was given by several simulation studies. In the present study, it is extended to the threedimensions by using a spherically symmetric 1-dimensional solution given by Parker. By using this model, we caninvestigate more detail about physically complex phenomena. We set this Parker solution and a dipole magneticfield to the initial conditions of the solar wind in the simulation. The three-dimensional structure of the solar windnear the sun has been simulated by using a three-dimensional global MHD model. The helmet-streamerconfiguration with a sharp boundary between the closed and open field regions has been demonstrated. At thattime, the solar wind speed in the open field regions is faster than that in the closed regions. Moreover a currentsheet is formed in the magnetic equatorial plane.

- 65 -

SB21-6

Study of CME Propagation in the Inner HeliosphereD. F. Webb1, T. A. Howard3, T. A. Kuchar1, J. S. Morrill5, R. A. Harrison6, C. J. Eyles8, R. A. Howard5, B.V. Jackson8, and J. C. Johnston2

1. Institute for Scientific Research, Boston College, Chestnut Hill, MA, USA2. Air Force Research Laboratory, Space Vehicles Directorate, Hanscom AFB, MA, USA3. Air Force Research Laboratory, Space Vehicles Directorate, Sunspot, NM, USA4. Physics Department, Montana State University, Bozeman, MT, USA5. Space Science Div., Naval Research Laboratory, Washington, D.C., USA6. Space Science and Technology Dept., Rutherford Appleton Laboratory, Chilton,7. Astrophysics and Space Research, University of Birmingham, Birmingham, UK8. CASS, University of California-San Diego, La Jolla, CA, USA

Results from an investigation of the propagation characteristics of coronal mass ejections (CMEs) using dataobtained by the Coriolis Solar Mass Ejection Imager (SMEI) and STEREO SECCHI imaging experiments on eachSTEREO spacecraft are presented. The LASCO and SECCHI COR1 and 2 coronagraphs observe the earlydevelopment of CMEs out to 30 Rs, or about 8 deg. elongation. The SECCHI Heliospheric Imager (HI)instruments, two on each STEREO spacecraft, have circular fields of view (FoVs) centered on the ecliptic plane,with HI-1 and -2 having FoVs 10 deg. and 35 deg. in radius, respectively. Their FoVs are designed to overlapwith each other and with the coronagraphs, essentially providing a continuous view of CMEs from the Sun to 1AU. SMEI is an all-sky imager that detects and tracks CMEs from elongations >20 deg. Thus, both HIs andSMEI have the potential to observe the same CME simultaneously. We discuss preliminary analyses of severalsuch events observed in 2007, in particular their kinematic and structural evolution out to ~100 deg. We presentresults from measurements of geometry and kinematic evolution as the transient evolves from the CME observedby coronagraphs to the I(nterplanetary)CME observed by the heliospheric imagers, and discuss implications forthe physics of their evolution. We also discuss the implications of these results for understanding the propagationof CMEs along the Sun-Earth line and, thus, for space weather.

- 66 -

SB22I-1

Stereo Observations of the Solar Corona from the SECCHI ExperimentAngelos Vourlidas

Code 7660, U.S. Naval Research Lab, Washington DC 20375, USA

The Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) on the NASA Solar TerrestrialRelations Observatory (STEREO) mission is a suite of remote sensing instruments consisting of an extremeultraviolet (EUV) imager, two white light coronagraphs, and two telescopes that comprise the heliospheric imager.SECCHI will observe coronal mass ejections (CMEs) from their birth at the sun, through the corona and into theheliosphere. A complete instrument suite is being carried on each of the two STEREO spacecraft, which willprovide the first sampling of a CME from two vantage points. The spacecraft, launched 25 October 2006, areorbiting the Sun, one Ahead of the Earth and the other Behind, each separating from Earth at about 22 degrees peryear. The primary science objectives are focused on understanding the physics of the CME process - theirinitiation, 3D morphology, propagation, interaction with the interplanetary medium and space weather effects. Byobserving the CME from multiple viewpoints with UV and coronagraphic telescopes and by combining theseobservations with radio and in-situ observations from the other instruments on STEREO as well as from othersatellites and ground based observatories operating at the same time, answers to some of the outstanding questionswill be obtained. All of the telescopes are working very well and have been producing spectacular images. Thepanoramic view of the inner solar system is unprecedented. We will show examples of some of the data and someof the initial results.

SB22-1

Solar Wind Structure - Origin and Solar Cycle DependenceMasayoshi Kojima, Munetoshi Tokumaru, Ken-ichi Fujiki, and Hiroaki Itoh

Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, 464-8601, Japan

We have studied the solar cycle dependence of solar wind properties and origins of the solar wind using IPS dataobtained at STELab over a solar cycle. The mean velocity at the polar region was stable with a speed of 789+/-68km/s throughout a solar cycle except for a few years around the solar maximum. When the polar coronal holeshrank to size smaller than critical scale size of about 5*10^10 km^2 in the solar maximum phase, it became thesource of slow solar wind. The fast and slow solar winds were separated with a steep velocity gradient, even if thescale of the high-speed region changed. The high-latitude fast wind had a N-S asymmetry in velocity, which was astable characteristic that lasted throughout the whole solar cycle we analyzed. The solar wind velocity, especiallyin the solar minimum phase, can be well predicted from a ratio of two coronal parameters (B/f): B is photosphericmagnetic field intensity and f is a flux expansion rate in corona.

- 67 -

SB22-2

How Magnetic Cloud Models Correspond to Clouds' Real Shapes andDimensions?M. Vandas1, A. Geranios2, and E. P. Romashets3

1. Astronomical Institute, Academy of Sciences, Bocni II 1401, 14131 Praha 4, Czech Republic2. Physics Department, University of Athens, Panepistimioupoli-Kouponia, Athens 15771, Greece3. Solar Observatory, Prairie View A & M University, Prairie View, TX, 77446, USA4. IZMIRAN, Russian Academy of Sciences, Troitsk, Moscow Region, 142190, Russia

Geometric parameters of magnetic clouds are commonly determined by fits of magnetic (and sometimes plasma)in-situ measurements to modelled profiles. Spacecraft measurements provide us only with quantities along aparticular line (trajectory) through an evolving magnetic cloud. Therefore various simplifying assumptions mustbe made on models, e.g. local approximation of the cloud by a cylinder with symmetry around the axis and alongit. It is difficult to verify independently obtained geometric parameters of the cloud like its axis orientation or itsdimensions, because we do not "see" needed quantities apart from the trajectory. On the other hand, MHDsimulations may provide us with such an information. Three-dimensional calculations of magnetic cloudpropagation give us a global view and, in addition, they can simulate what a hypothetic spacecraft would measurewhen crossing a cloud. The paper will present comparisons of model fits with real shapes of magnetic cloudswhich can be directly obtained from our simulations.

SB22-3

Solar Cycle Changes in 3-D Solar Wind - Consequences on Space WeatherP.K. Manoharan

Radio Astronomy Centre, National Centre for Radio Astrophysics, TIFR, Ooty 643001, India

This paper reviews some of the space weather science projects under the `Indian CAWSES and IHY Programs'. Itpresents results on evolution of three-dimensional solar wind flows: (1) steady fast streams originating above theopen field coronal holes, (2) variable low-speed flows near the closed corona associated with active regions and(3) transients caused by the interaction of slow and fast streams and fast coronal mass ejections in response to thesolar activity over the solar cycle #23. The primary solar wind data set for this study has been obtained from theOoty Radio Telescope (India), which is capable of observing the interplanetary scintillation of a large number ofradio sources (about 800-1000 radio sources) every day. These measurements provide the three-dimensionalimages of the solar wind density and speed in the sun-earth distance range. The result indicates that theinteractions caused by the recurrent and high speed streams during the year 2003 are among the most dominant ofthe entire solar cycle in producing the enhanced level of density turbulence and in causing the geoeffectiveness.The observed changes in solar wind disturbances are discussed with an emphasis on the radial evolution of thethree-dimensional structure of the inner heliosphere over the solar cycle. This presentation will also cover some ofthe results of observations taken during the CAWSES-India campaign.

- 68 -

SB22-4

A Magnetohydrodynamic Turbulence Model Predicitng the RadialEvolution of Solar WindsNobumitsu Yokoi

Institute of Industrial Science, University of Tokyo, Japan

A magnetohydrodynamic (MHD) turbulence model that can describe the radial evolution of the solar wind isproposed. In the model, the equations of the mean velocity and magnetic fields are solved simultaneously with thedynamics of the turbulent statistical quantities. As for the turbulent quantities that represent statistical propertiesof turbulence, we adopt the turbulent MHD energy, its dissipation rate, the cross helicity (velocity/magnetic-fieldcorrelation), and the turbulent MHD residual energy (the difference between the kinetic and magnetic energies).Like other pseudo-scalar quantities such as the kinetic and magnetic helicities, the cross helicity is of fundamentalimportance in describing the generation of the global magnetic field and the suppression of the momentum andscalar transports in plasma turbulence. Linked with the outward propagating Alfven waves, the solar-windfluctuation shows a high cross-correlation between the velocity and magnetic fields. No other MHD phenomenaexhibit such a high correlation. We also examine the mechanisms that supply various helicities to the solar-windturbulence. Shears in the mean velocity and magnetic fields associated with the boundaries of the low-speedstream (LSS) and the high-speed stream (HSS) and boundaries of the magnetic sectors are representative factors.These points suggests various helicities including the cross helicity can play important role in the evolution of thesolar-wind turbulence. This model is expected to provide a useful tool for predicting the solar-wind behavior inthe Sun-Earth system.

SB22-5

Observations of Interplanetary and Ionospheric Scintillation UsingMulti-beams Big Scanning ArrayIgor V. Chashei, Vladimir I. Shishov, Sergei A. Tjul'bashev, and Il'nur A. Subaev

lebedev Physical Institute, Pushchino Radioastronomy Observatory, Russia

Technique and data reduction are described of interplanetary plasma monitoring using observations ofinterplanetary scintillation (IPS) at Big Scanning Array of Lebedev Physical Institute (frequency 111 MHZ).Ionospheric scintillation (ISS) are observed simultaneously with IPS. We observe and analyzed daily IPS and ISSof the whole statistical ensemble of radio sources passing the array diagram. Results are presented obtained in theframe of monitoring program during the years 2003-2007 as for quiet so for disturbed conditions.

- 69 -

SB22-6

Solar Wind Propagation Delay Dependence on Heliospheric StructureLee Frost Bargatze

Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567, USA

The temporal response of magnetospheric activity to variations of solar wind conditions upstream of the Earthrequire the use of a solar wind propagation correction (SWPD) model to account for the time delay associatedwith solar wind parcel transit from an upstream monitor to the bow shock of the magnetosphere. New advancedmodels that account for SWPD have only recently superceded simple models such as the X/V radial convectionmodel. The Weimer et al. [2002] SWPD model is based on the assumption that solar wind phase front normaldirections can be found by synchronizing the IMF time series from at least three solar wind monitors. Here, solarwind phase fronts are nearly planar surfaces (on the scale of hundreds of Earth radii) in which the IMFinformation content, that is, vector direction and temporal variation, is highly correlated. A SWPD techniquebased on observations from a single monitor can also be used to estimate solar wind phase plane orientation viaconstrained minimum variance analysis on one IMF data time series. A survey of phase plane normal orientationstatistics compiled over the last eight years reveals that the phase front normals tend to cluster as if beamed in afew isolated directions that change from one solar rotation to the next. The normal directions are by no meansconfined to the ecliptic plane. The results of a search for empirical connections between coronal magnetic fieldevolution and condition upstream of the Earth will be presented.

SB22-7

Solar-Wind Sources for Large-Scale Disturbances during GeomagneticStormsLarry Lyons1, Shasha Zou1, Dae-Young Lee2, Chi-Ping Wang1, and Stephen Mende3

1. Department of Atmospheric and Oceanic Sciences, University of California, Los Angeles, Los Angeles, CA 90095-1565,USA2. Department of Astronomy and Space Science, College of Natural Sciences and Institute for Basic Science Research,Chungbuk National University, Korea3. University of California, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720-7450, USA

We have previously identified different types of IMF and solar wind changes that lead to disturbances and featuresof the resulting disturbances. Here we use global auroral images, geosynchronous particle data, and groundmagnetometer observations to focus on unusually large-scale storm-time disturbances, including sawtooth eventdisturbances and super substorms during the storm main phase of severe storms. We find that pressure triggeringis critical for understanding these disturbances, and that pressure increases are more likely to lead to substormdisturbances under strongly southward IMF conditions such as occur during storms than during other conditions. This offers an explanation for the global nature of many stormtime disturbances because pressure increases understrongly southward IMF cause a two-mode disturbance: global compression and a nightside substorm, and bothincrease the aurora and energetic particles. Additionally, we find evidence that with extremely large |By| orextremely large negative Bz, the normal requirement for prolonged (>1 hr) southward IMF may not be necessaryfor there to be a pressure triggered substorm.

- 70 -

SB31I-1

Radiation Belt ClimatologyYoshizumi Miyoshi1 and Ryuho Kataoka2

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, JAPAN2. RIKEN (The Institute of Physics and Chemical Research), Saitama 351-0198, JAPAN

We examined long term variations of energetic particles in the radiation belts using data from the NOAA(1979-2006) satellites. We found a significant flux variation and variations of peak L-value during the solar cyclewith both semiannual and recurrent 27 and 13.5 days flux variations. The outer radiation belt moves toward theearth during the solar maximum, while it moves outward during the solar declining phase. We conducted thenumerical simulation of radial diffusion that changes the diffusion coefficient. The simulation reproduced thelong-term variation of peak L-shell of the outer belt.

SB31I-2

Long-term Variations of Auroral Acceleration Region and InnerMagnetosphere Region Observed by the Akebono SatelliteA. Kumamoto1, T. Ono1, M. Iizima1, A. Morioka1, and H. Oya2

1. Department of Geophysics, Tohoku University, Aoba, Aramaki, Aoba, Sendai, 980-8578, Japan2. Department of Space Communication Engineering, Fukui University of Technology, 3-6-1 Gakuen, Fukui, 910-8505, Japan

The Akebono (EXOS-D) satellite has performed observations of electric field, magnetic field, energetic particles,plasma waves, and auroral images in the polar ionosphere and the inner magnetosphere. 18 years' worth of plasmawave data obtained by the Akebono satellite enables us to understand the long-term behavior of the auroralpotential drops in the polar region and dynamics of the plasmasphere. Based on the analyses of the auroralkilometric radiation (AKR), which is generated by auroral electron precipitations in the polar region, it has beenfound that AKR activity varies depending on seasons and solar cycle: AKR is more active in the winter polarregion than in the summer polar region [Kumamoto and Oya, 1998]. AKR during solar maximum is weaker thanthat during solar minimum [Kumamoto et al. 2003]. The phenomena suggest that some conditions of theionosphere, which vary depending on the solar zenith angle and solar EUV flux, control the auroral potentialdrops and AKR sources locating far above the ionosphere. It has also been indicated by long-term upper hybridresonance (UHR) wave data that plasmasphere structure dynamically varies depending on geomagnetic activities:The plasmasphere rapidly shrinks during the storm main phase and gradually extends during the storm recoveryphase. During recovery phase, irregular structures also often appear. The solar cycle variation of electron numberdensity, Ne, is seen only within L<2 in the plasmasphere. As for the variations of Ne in L>2 and the location ofplasmapause, Lpp, geomagnetic activity, or magnetospheric convection strength, seems to be the dominant controlfactor.

- 71 -

SB31I-3

Empirical Approach to Modeling the Dynamical Trapped RadiationEnvironmentShing F. Fung

Heliospheric Physics Laboratory, Code 672, NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA

Since the development of the NASA AP/AE 8 trapped radiation models, the de facto standard empirical modelsfor Earth's radiation belts, it has become clear that these models are deficient in capturing the dynamical changesof the radiation belts resulting from geomagnetic variability. Consequently, physics-based modeling has becomethe focus in the last few years to gain understanding of radiation belt processes. Despite significant advances fromstudies of the acceleration, diffusion and loss processes, accurate and practical physics-based models of theradiation belts are not yet available. This presentation will consider how empirical techniques might be employedto model the variable trapped radiation environment. The requirements of long-term database that might beneeded to support empirical modeling, and how empirical modeling techniques can complement physicalmodeling will be discussed.

SB31-1

Acceleration of Relativistic Electrons in the Process of Whistler-modeChorus GenerationYuto Katoh1 and Yoshiharu Omura2

1. Planetary Plasma and Atmospheric Research Center, Graduate School of Science, Tohoku University, Japan2. Research Institute for Sustainable Humanosphere, Kyoto University, Japan

We study acceleration of resonant electrons in the generation process of whistler-mode chorus emissions by aself-consistent particle code. The present study clarifies that the role of nonlinear wave trapping is significant inthe energizing process of relativistic electrons by narrowband whistler-mode chorus emissions. Whistler-modechorus emissions are electromagnetic plasma waves which consist of narrow band elements with rising tonesobserved in the dawn side of the Earth's magnetosphere. Results of in situ observations have revealed that thechorus emissions are generated from the equatorial region of the magnetosphere and that its activity is enhancedduring geomagnetically disturbed peorids. Theoretical analyses have also suggested that the generation process ofchorus emissions is deeply related to the nonlinear cyclotron resonant interaction with energetic electrons in anon-uniform magnetic field.Recently we have reproduced the generation process of chorus emissions by a large-scale particle simulation[Katoh and Omura, 2007]. We find that a fraction of resonant electrons having large pitch angle are energizedthrough nonlinear wave trapping by chorus emissions while the majority of electrons lose energy contributing tothe generation of chorus emissions. Simulation result reveals that selected trapped electrons are effectivelyaccelerated over 100 keV during 2500 gyro-periods. We also find a characteristic behavior of highly acceleratedelectrons showing a turning of direction from equatorward to poleward during the acceleration process, which isexplained by the relativistic turning acceleration (RTA) process theoretically analyzed by Omura et al. (2007).

- 72 -

SB31-2

The Origin of Metric Type II BurstsNariaki V. Nitta

LMSAL, USA

Type II radio bursts result from plasma emission by shock-accelerated electrons. For type II bursts observed inthe decametric-hectometric (DH) and kilometric ranges, the driver of the shocks should be fast coronal massejections (CMEs). However, whether CMEs are responsible also for metric type II bursts is still a subject ofcontroversy. This partly reflects the intimate (but not-fully-understood) relationship between CMEs and flares. Conversely, studies of metric type II bursts in comparison with their DH and kilometric counterparts as well aswith other related phenomena such as EIT waves have a great potential to clarify various aspects of the CME-flarerelation. These studies may also be useful for understanding the variabilities of some of the hazardous solarenergetic particle (SEP) events. Here we start from matching various lists and catalogs to conduct a statisticalstudy of possible associations of metric type II bursts during 1996-2006 with CMEs and flares. This is followedby a detailed study of a subset of well-observed events, including an examination of lower coronal andcoronagraphic images and radio spectra, to address the question of whether the rich variety of the appearances ofmetric type II bursts arises from varieties of the CME-flare relation.

SB31-3

Efficiency of Particle Acceleration in Geospace and Its Role in Storm-timeRing Current Development and Radiation Belt EnhancementIoannis A. Daglis1, Fiori-Anastasia Metallinou1, Thomas E. Moore2, Mei-Ching Fok2, Marina Georgiou1, and Athina Varotsou3

1. National Observatory of Athens, Institute for Space Applications and Remote Sensing, GR-15236 Penteli, Greece2. Laboratory for Geospace, NASA Goddard SFC, Greenbelt, MD 20771, USA3. Los Alamos National Laboratory, ISR-1, Los Alamos, NM 87545, USA

Particle acceleration is the central physical process of space weather phenomena in the terrestrial magnetosphere.Its efficiency determines to a large extent the character and dynamice evolution of the major disturbancephenomena in geospace, i.e. geospace magnetic storms and magnetospheric substorms, and their space weatherproducts, i.e. the storm-time ring current development and the radiation belt enhancement. Here we are presentingand discussing results of acceleration modeling and data analysis pertinent to ring current and radiation beltenhancement. The role of solar wind-magnetosphere coupling and magnetosphere-ionosphere coupling insynergistically driving particle acceleration is the main guiding line of this paper.

- 73 -

SB32-1

Monitoring the Plasmaspheric Plasma Density with MAGDAS/CPMNMagnetometer NetworkHideaki Kawano1, Shuji Abe2, Satoko Takasaki3, Naoya Maeda1, and Kiyohumi Yumoto2

1. Department of Earth and Planetary Sciences, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan2. Space Environment Research Center, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan3. National Institute of Polar Research, 9-10, Kaga 1-chome, Itabashi-ku, Tokyo 173-8515, Japan

From the ground, one can monitor the plasmaspheric plasma density; one can do so by identifying the field-lineresonance (FLR) signature in ground magnetometer data. The FLR causes eigenoscillations of geomagnetic fieldlines, and the eigenfrequency of a field line depends on the field strength and the plasma mass density along thefield line. Thus, by using a model of the geomagnetic field, one can estimate the plasmaspheric plasma massdensity from the observed field-line eigenfrequency, if the field line in question is located inside theplasmasphere.In this paper we present cases in which we monitored the plasmaspheric plasma density by using the data fromMAGDAS/CPMN (MAGnetic Data Acquisition System/Circum-pan Pacific Magnetometer Network), includingthe following. We also discuss possible future directions.Takasaki et al. (2006) observed FLR at L~1.4, from which they reported an increase in the equatorial plasmadensity at L~1.4 during a large storm. This is surprising, because it is usually thought that the plasmasphereshrinks during a storm; Takasaki et al. interpreted the increase in terms of an outflow of heavy ions (e.g., O+)from the ionosphere to the plasmasphere.Abe et al. (2006) observed FLR at L~5.8, and compared the FLR-based density estimates with the He+ columnabundance at the same point (field-aligned mapped to the equator) observed by the Extreme Ultraviolet Imageronboard the IMAGE satellite. As a result, they found coherent time-dependent changes in the two data as theobservation site moved through a plasmaspheric plume.

SB32-2

Penetration of Magnetospheric Electric Fields to the Equator during aGeomagnetic StormTakashi Kikuchi1, Kumiko K. Hashimoto2, and Kenro Nozaki3

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan2. Kibi International University, Takahashi, Okayama 716-8508, Japan3. National Institute of Information and Communications Technology, Koganei, Tokyo 184-8795, Japan

Penetration of the magnetospheric electric field to the equatorial ionosphere was examined for the geomagneticstorm on November 6, 2001, by analyzing the difference in magnitude of the geomagnetic storm recorded at thedayside dip equator, Yap and low latitude, Okinawa. The electric field caused DP2 currents at the equator duringthe storm main phase. The ring current started to develop simultaneously with the equatorial DP2, which impliesprompt transmission of the convection electric field to the inner magnetosphere as well as to the equatorialionosphere. The equatorial DP2 turned to the counter electrojet (CEJ) in the beginning of the storm recoveryphase, when the southward IMF decreased its intensity. The shielding electric field became effective one hourafter the onset of the storm, and was dominant enough to cause the CEJ during the recovery phase. The westwardauroral electrojet in the dawn sector was driven over subauroral latitude centered at 57 degs CGML during themain phase, while the AEJ shifted rapidly to the auroral latitude centered at 67 degs CGML in the beginning ofthe recovery phase. It is concluded that the electric field associated with the DP2 currents contributed to thedevelopment of the ring current, while the overshielding electric field may have contributed to cease developingthe ring current. The overshielding must be caused by the abrupt poleward shift of the R1 FACs in addition to thedecrease in their magnitude, resulting in predominance of the shielding electric field due to the R2 FACs.

- 74 -

SB32-3

KRM Modeling for Space Weather Specifications of the Polar IonosphereAki Ieda and Y. Kamide

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8601, Japan2. Research Institute for Sustainable Humanosphere, Kyoto University, Uji 611-011, Japan

The Kamide-Richmond-Matsushita (KRM) method is a magnetogram-inversion modeling algorithm to specify theearth's polar ionosphere. The space weather maps generated by KRM provides spatial information of ionosphericvariables, in contrast to scalar geomagnetic indices such as AE, Dst, and Kp. KRM assumes Ohm's law for theionosphere, deriving ionospheric parameters including electric fields and field-aligned currents primarily fromobserved ground magnetic field perturbations along with observed or modeled ionospheric conductance. Thereal-time operation of KRM (http://gedas.stelab.nagoya-u.ac.jp/) displays nowcasting of the ionosphere. In thispresentation, we will demonstrate how KRM results can be improved by using conductances derived from globalauroral images.

SB32-4

Substorm Growth Phase and Onset MechanismC. Z. Cheng1, Sorin Zaharia2, N. Gorelenkov3, and T. F. Chang1

1. Plasma and Space Science Center, National Cheng Kung University, Taiwan2. Los Alamos National Laboratory, MN, USA3. Princeton Plasma Physics Laboratory, Princeton University, NJ, USA

The Earth's magnetosphere and ionosphere during substorms evolve typically from the growth phase to substormonset to the expansion phase and then to quiet time states. During different phases of substorms themagnetosphere and ionosphere exhibit distinct 3D global and local features. Successful theories or models forunderstanding substorm dynamics must provide physical understanding of these features. Here, we describe theevolution of 3D global structure of the magnetosphere during the growth phase and ULF (in the Pi 2 frequencyrange) instabilities that are excited a few minutes prior to onset to produce the auroral arc that breaks up after thesubstorm onset. The 3D structure of global magnetosphere during growth phase is modeled by quasi-staticequilibrium solutions obtained from the force-balance equation for given equatorial pressure distributions. TheULF instability responsible for the breakup auroral arc is modeled by the Kinetic Ballooning Instability (KBI),which is destabilized by plasma pressure gradient and magnetic field curvature in the high beta magnetic wellregion in the near-Earth plasma sheet. Our model is based on the theoretical analysis and numerical solutions ofthe gyrokinetic mode equations for late growth phase 3D magnetospheric equilibria. The results show that the KBIhas a real frequency associated with the ion magnetic drift frequency, which is in the Pi2 frequency range, and themost unstable KBI has an azimuthal mode number on the order of 200-300. The theoretical KBI features areconsistent with observational features in both the aurora breakup arcs and the near-Earth plasma sheet. During theexpansion phase the plasma pressure profile is relaxed due to plasma transport by strong plasma turbulence and itcan be shown that the plasma sheet magnetic field becomes depolarized resulting from a small reduction in theplasma pressure. Comparison between our model and substorm observations will be presented.

- 75 -

SB32-5

Recent Observations of ULF Waves Relevant to Geomagnetic Storms,Radiation Belts, and the Ring CurrentMark J. Engebretson1 and Ian R. Mann2

1. Augsburg College, Minneapolis, MN 55454 USA2. University of Alberta, Edmonton, AB T6G 2E1 Canada

Many studies in recent years have highlighted the importance of ULF waves in contributing to major changes inthe population of energetic particles in Earth’s magnetosphere. These include acceleration and radial transport ofrelativistic electrons in the outer radiation belt by long-period (Pc 5) waves, as well as interactions withelectromagnetic ion cyclotron waves (Pc 1-2) that cause pitch angle scattering and consequent loss of both ringcurrent ions and (via parasitic interactions) relativistic electrons. We review here some recent observations, fromboth the ground and from space, that offer new insights into the interactions that regulate these particle fluxes. These include insights made possible by the use of a ULF index, new studies that address apparent contradictionsbetween ground-based and space-based observations of EMIC waves during magnetic storms, and studies of thecharacteristics of Pc 5 and EMIC waves during superstorms.

SB32-6

Development of the Solar-Terrestrial Environment Integrated SimulatorH. Shinagawa1, H. Shimazu1, N. Terada1, H. Jin1, Y. Kubo1, K. Fukazawa1, K. Tsubouchi1, T. Obara1, H. Fujiwara2, S. Fujita3, Y. Miyoshi4, A. Nakamizo4, and T. Tanaka4

1. National Institute of Information and Communications Technology, Tokyo 184-8795, Japan2. Tohoku University, Sendai 980-8578, Japan3. Meteorological College, Kashiwa 277-0852, Japan4. Kyushu University, Fukuoka 812-8581, Japan

The solar-terrestrial system consists of the solar atmosphere, the interplanetary space, the earth's magnetosphere,the ionosphere, and the neutral atmosphere. Those regions have different physical characteristics and phenomenawith different temporal and spatial scales. In particular, the magnetosphere, the ionosphere, and the neutralatmosphere are strongly coupled with each other, and interaction between the regions is nonlinear and extremelycomplicated. Even within each region, there are strong interactions between physical processes with differenttemporal and spatial scales. Furthermore, the geospace environment significantly varies as electromagnetic energyand particles from the sun vary. In order to quantitatively understand the solar-terrestrial environment, it isnecessary to model the sun-earth system by including fundamental processes self-consistently. Although manykinds of global numerical models of the geospace have been constructed and used to study geospace disturbances,most of them focus on the effects of the solar origin. However, recent observations have indicated thatatmospheric waves generated in the lower atmosphere significantly influence the upper atmosphere, theionosphere, and possibly the magnetosphere. We have been developing an integrated simulation model of thesolar-terrestrial system, which self-consistently includes the entire region between the solar surface and the earth'ssurface. It is expected that the model will enable us to understand physical processes of the system by includingnot only effects of the disturbances from the sun on the geospace environment, but also effects of themeteorological phenomena on the upper atmosphere. We will report the status of the model development, andpresent preliminary results.

- 76 -

SB41I-1

Modeling of Flares and CMEsTerry G. Forbes

University of New Hampshire, USA

The occurrence of eruptions in the solar atmosphere has been known for more than a 150 years, yet the underlyingmechanism that creates them remains uncertain. Most present-day models for these eruptions are based on theprinciple that the energy that drives them comes from the free magnetic energy associated with electrical currentflows in the solar corona. However, there is no general agreement as to what causes the rapid release of thisenergy at the onset of an eruption. One possibility is that the energy release is caused by a combination of ideal(loss of a stable equilibrium) and non-ideal (magnetic reconnection) processes. The first process can explain therapid onset of the eruption, but the second is needed to explain the large scale of the energy release. Severalresearch groups around the world are currently developing three-dimensional models based on these twoprocesses.

SB41-1

Tracking Interplanetary Shock Waves by using Global Three-DimensionalNumerical Simulations: 12 May 1997; Halloween 2003; and 5-6 December2006Chin-Chun Wu1, Murray Dryer2, C. D. Fry3, and S. T. Wu1

1. CSPAR, University of Alabama, Huntsville, Alabama 35899, USA2. NOAA/SEC, Boulder, Co 80305, USA3. Exploration Physics International, Inc., Huntsville, AL 35806, USA

This study performs simulations of interplanetary coronal mass ejection (ICME) propagation in a realistic 3Dsolar wind structure from the Sun to the Earth and beyond by using the newly developed hybrid code,HAFv.2+3DMHD (Wu et al., 2007). This code combines two simulation codes: Hakamada-Akasofu-Fry codeversion 2 (HAFv.2) which simulates solar wind structures from source surface maps out to 18 solar radii (Rs); anda fully three-dimensional, time-dependent MHD simulation code which simulates solar wind structures from 18Rs (by taking the output of HAFv.2 as the input at 18 Rs) out to the Earth and beyond. In order to compare withWIND/WAVES (or STEREO/WAVES) Type II observations, plasma frequency is also derived from simulationresults to track the location of interplanetary shock waves. Events that occurred in both low and high solar activityperiods will be presented (e.g., the famous events of May 12, 1997 and October-November 2003). Several recentevents will also discussed (e.g., December 5-6, 2006).

REFERENCE: Wu, C.-C., C. D. Fry, S. T. Wu, M. Dryer, and K. Liou, Three-dimensional global simulation ofICME propagation from Sun to the heliosphere, J. Geophys.

- 77 -

SB41-2

Fine Auroral Structures and Dynamics and Their Relationship to theAuroral Particle Signatures Observed by the Reimei SatelliteMasafumi Hirahara1, Takeshi Sakanoi2, Kazushi Asamura3, Yasuyuki Obuchi2, Atsushi Yamazaki3, Kanako Seki4, Yusuke Ebihara4, Yasunobu Ogawa5, Yasumasa Kasaba2, Yukinaga Miyashita3, and Iku Shinohara3

1. Department of Eath and Planetary Science, University of Tokyo, Tokyo, Japan2. PPARC, Tohoku University, Sendai, Japan3. ISAS/JAXA, Kanagawa, Japan4. STEL, Nagoya University, Nagoya, Japan5. National Institute of Polar Research

The Reimei satellite is the first state-of-the-art micro satellite of ISAS/JAXA, whose scientific capability wasdesigned and dedicated for the novel observations of fine auroral structures and dynamics from an altitude ofabout 640 km. The sun-synchronous orbit in the noon-midnight meridian is pretty suitable for the repeatedobservations of nightside auroral activities and dayside cusp phenomena. Reimei carries three selections ofscientific instruments: multi-spectral auroral imaging camera, electron and ion energy spectrum analyzers, and theplasma current monitor, all of which have the high-time and -spatial resolution performance matching thescientific purpose. The auroral imaging camera can take images of an area of about 70x70 square km every 120msec with 64x64 pixels independently for three wavelengths of 428, 558, and 670 nm. The top-hat type energyspectrum analyzers for electron and ion are able to cover both energy range of 12 eV to 12 keV and almost fullpitch angle range every 20 msec owing to the precise satellite attitude control based on the local magnetic fieldmeasurement. The simultaneous observations using the auroral camera and electron/ion analyzers have indicatedthat there are several distinctive features concerning the auroral emissions and the related auroral particledistribution even in one auroral structure. In this presentation, we address typical observational propertiesobserved by Reimei, as represented by the followings.1) Active auroral arc/band structure corresponding to the auroral electron precipitation caused by the upwardparallel electric field2) Microscopic (fast and repetitious) energy-dispersing electron signatures probably related with kinetic Alfvenwave activity3) Ion precipitation accelerated by the downward parallel electric field at the vicinity of the Inverted-V electronsignatures4) Ion upflows and accelerated ions of ionospheric origin in the dayside cusp region5) Black auroras correlated with the lack of high-energy electron components in Inverted-V structure6) Pulsating auroras associated with quasi-periodic precipitation of high-energy electronsIt is also planned to demonstrate the utility for the data analysis tool at the presentation site.

- 78 -

SB41-3

Study of Geotail Observations of FTEsG. I. Korotova1 and D. G. Sibeck2

1. IZMIRAN, Troitsk, Moscow Region, 142190, Russia2. NASA/GSFC, 8800 Greenbelt Rd, Greenbelt, MD 20723, USA

We present the results of a study of FTEs observed by Geotail for 3.5 years. We describe plasma flowperturbations in the outer magnetosphere during the passage of cylindrically shaped flux transfer events. We consider predictions of fluid dynamic theory for Bn and Vn signatures of FTEs. Event boundaries can bedistinguished by sharp reversals in flow directions. We determine direction of event motion in dependence onsense of polarity of Bn component of FTEs. We study the motion of events within the magnetosheath that movefaster or slower relative to the magnetosheath flow itself and the signatures that they produce in plasmaparameters. We present the distribution of Vn amplitudes for sheath and sphere FTEs. We present some examplesof FTEs and the results of a survey of plasma signatures of FTEs observed by Geotail.

SB41-4

Continuous Transition from Fast to Slow Regime of Magnetic Reconnectionand Application to Solar FlaresShin-ya Nitta

1. Hinode Science Center, National Astronomical Observatory of Japan2. Interactive Research Center of Science, Tokyo Institute of Technology3. Department of Information and Communication Engineering, The University of Electro-Communications

This paper analytically investigates a series of two-dimensional MHD reconnection solutions over a large range ofmagnetic Reynolds number (Rem*). A new series of solutions explains a continuous transition from Petschek-likefast reconnection to a much slower regime with a longer current sheet, in which the inflow region is obtained froma Grad-Shafranov analysis (Nitta et al. 2002) and the outflow region from a shock-tube approximation (Nitta2004, 2006). A Petschek-like solution (with a single X-point) forms for a sufficiently small Rem*. As Rem*gradually increases, the solution shifts to an X-O-X solution with an O-point between two X-points. When Rem*increases further, the island collapses to a new longer current sheet with Y-points at its ends. As Rem* increases,the reconnection rate slows and the reducible fraction of the initial magnetic energy of the system decreases.These reconnection structures expand self-similarly with time.

- 79 -

SB41-5

Dayside Magnetic Reconnection during the Northward IMFKyung Sun Park1, Tatsuki Ogino2, and Yong Ha Kim1

1. Dept, of Astronomy and Space Science, Chungnam National University, Daejeon 305-764, Korea2. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan

We have performed a high-resolution and time-dependent three dimensional MHD simulation of interactionbetween the solar wind and the Earth's magnetosphere when the dipole tilt and northward IMF are simultaneouslyincluded in the whole volume of simulation box. In present study, for the case of positive dipole tilt, threedifferent characteristics of reconnection region appear at the dayside magnetopause during the northward IMFconditions; 0 deg < theta < 60 deg, 60 deg < theta < 120 deg and 120 deg < theta < 180 deg, where theta is acounterclockwise angle from the Y-axis in a view from the sun. In the northern and southern hemispheres, boththe electric field in the direction of convection and the resistive electric field are largest in the region where wewould expect occurrence of antiparallel reconnection. Moreover the electric field in the northern hemisphere isalmost 3 times larger than that in the southern hemisphere for 45 deg < theta. However the parallel component ofthe current in the southern hemisphere is larger than northern hemisphere when the dipole tilt is positive. Thefeature is different from that for southward IMF condition [Park et al., 2006]. In addition, the perpendicularvorticity has large value in the reconnection regions.

SB41-6

Pulsive Jets in Three-Dimensional Fast Magnetic ReconnectionTohru Shimizu1, Koji Kondo1, Kazunari Shibata2, and Masayuki Ugai1

1. Ehime University, Dept. of Compuer Science, Bunyo 3, Matsuyama City, 790-8577, Japan2. Kwasan Observatory, Graduate School of Science, Kyoto University, Kyoto City, 607-8471, Japan

Three-dimensional instability of the spontaneous fast magnetic reconnection is studied with MHD (MagnetoHydro Dynamic) simulation. It is shown that the classical two-dimensional model of the spontaneous fastmagnetic reconnection in which the magnetic neutral point and plasmoid are considered to be unlimitedlyextended in the sheet current direction is unstable for a resistive perturbation in the sheet current direction. Then,the reconnection process is spontaneously localized in the sheet current direction and self-organized to generatestrong reconnection jets. As a result, three-dimensional plasmoids are intermittently ejected from the reconnectionregion. The generation of the three-dimensional plasmoids are random and pulsive. This study is applied to thereal space observation data of sun and earth.

- 80 -

SB41-7

Three Dimensional Magnetohydrodinamic Simulation of Coronal MassEjectionsD. Shiota1, K. Kusano2, T. Miyoshi3, N. Nishikawa4, and K. Shibata5

1. Center for Computational Astrophysics, National Astronomical Observatory of Japan, JAPAN2. The Earth Simulator Center, Japan Agency for Marine-Earth Science and Technology (JAMSTEC), JAPAN3. Facility of Science, Hiroshima University, JAPAN4. Super Computer System Planning and Operations Department, JAMSTEC, JAPAN5. Kwasan and Hida Observatories, Kyoto University, JAPAN

Coronal mass ejections (CMEs) are one the most spectacular explosive phenomena, in which large amount ofmass and magnetic flux are ejected to the inter planetary space, as a result of a disruption of coronal magneticfield. They are one of the most important phenomena for space weather science because they are closely related tosolar energetic particles and geomagnetic storms.Recent observations by solar satellites revealed that CMEs are closely related to solar flares. However, all CMEdoes not have the corresponding flare, and vice versa. The relation between CMEs and flares remains still unclear.The reason is that, while flares are phenomena governed by only magnetic field structure in active regions, CMEsare complex phenomena which interact not only with magnetic field in active regions and their surrounding butalso with the gravity and the solar wind. Numerical simulation including both a local active region and the globalstructure such as solar wind structure is most efficient way to understand the inital processes of CMEs. In this study, we performed three-dimensional magnetohydrodynamic (MHD) simulations of an initiation of aCME in spherical geometry. We performed the simulation with wide parameter ranges in order to clarify thecondition for a flux rope to be ejected as a CME, we will report the detail of the numerical results in this paper.

- 81 -

SB42I-1

Space Weather Modeling on the Solar Flare Event in December 2006 (1):From the Sun to Interplanetary SpaceK. Kusano1, K. Shibata2, R. Kataoka3, S. Inoue4, D. Shiota5, E. Asano2, T. Matsumoto2, T. Miyoshi6, T. Ogino4, and the Modeling Task Force Group

1. The Earth Simulator Center, Japan Agency for Marine-Earth Science and Technology, Japan2. Kwasan Observatory, Kyoto University, Kyoto, Japan3. RIKEN (The Institute of Physics and Chemical Research), Japan4. Solar Terrestrial Environmental Laboratory, Nagoya University, Japan5. National Astronomical Observatory of Japan6. Hiroshima University, Japan

The numerical modeling of space weather phenomena is crucially important for the understanding of solarterrestrial connection mechanism as well as for the prediction of space weather influence. Based on the CreativeScientific Research "The Basic Study of Space Weather Prediction," we have tried to develop a holistic modelingof a series of space weather phenomena, which was initiated by the solar flare occurred in December 13, 2006 andcaused the strong geomagnetic impact. The model consists of the interlocked different simulations, which cancalculate the onset of solar flare, the formation of coronal mass ejection (CME), the propagation of interplanetaryCME (ICME), and the geomagnetic impact, respectively. First, we performed the so-called "data-driven" three-dimensional magnetohydrodynamic (MHD) simulation ofactive region NOAA10930, using vector magnetogram observed by Solar Optical Telescope (SOT) on boardHinode. Second, using the results of this active region model as the boundary condition of the global coronamodel, the formation of CME was investigated. Finally, the result of the global corona model was transmitted tothe interplanetary model, which simulated the propagation of ICME.This paper corresponds to the first part of our study, and the second half part is presented by Ogino, et al. for theconnection from interplanetary space to earth. Based on the results, the predictability of space weather processeswill be discussed.

SB42I-2

Numerical Simulations of the Initiation and the IP Evolution of CoronalMass EjectionsStefaan Poedts

Coronal Mass Ejections (CMEs) belong to the most violent and fascinating events in the solar system. These events involve large-scale changes in the coronal structure and significant disturbances in the solar wind.Especially the massive, fast CMEs are interesting to study as these events cause shocks that propagate through theinterplanetary (IP) space. In these IP shock waves energetic particles continuously accelerate giving rise togradual solar energetic particle events (SEPs). As a result, CMEs and the CME generated shock waves play a keyrole in the so-called space weather. Better mathematical models of the solar corona and of CME initiation eventsand IP CME evolution are required.We present recent results from numerical simulations of the initiation and IP evolution of CMEs in the frameworkof ideal magnetohydrodynamics (MHD). As a first step, the magnetic field in the lower corona and thebackground solar wind are reconstructed.Both simple, axi-symmetric (2.5D) solar wind models for the quiet sun as more complicated 3D solar windmodels taking into account the actual coronal field through magnetogram data are reconstructed. In a second step,fast CME events are mimicked by superposing high-density plasma blobs on the background wind and launchingthem in a given direction at a certain speed. In this way, the evolution of the CME can be modeled and its effectson the coronal field and background solar wind studied. In addition, more realistic CME onset models have beendeveloped to investigate the possible role of magnetic foot point shearing and magnetic fluxemergence/disppearence as triggering mechanisms of the instability.Parameter studies of such onset models reveal the importance of the background wind model that is used and ofthe initiation parameters, such as the amount and the rate of the magnetic flux emergence or the region and the

- 82 -

amount of foot point shearing.

SB42-1

Solar Flare Magnitude Forecast from Photospheric Magnetic FieldPropertiesTetsuya T. Yamamoto1, Takashi Sakurai1, Kanya Kusano2, and Takaaki Yokoyama3

1. National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan2. Earth Simulator Center, Japan Agency for Marine-Earth Science and Technology, 3173-25 Showa-machi, Kanazawa-ku,Yokohama, Kanagawa 236-0001, Japan3. Dept. of Earth and Planetary Physics, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku,Tokyo 113-0033, Japan

The solar flare is a transient phenomenon, and has great influence on the sun-earth environment. It is important toforecast when, where and how a large flare occurs.In this study, we compared solar flare magnitudes and photospheric magnetic properties quantitatively for thepurpose of forecasting how large a flare may be. We applied a linear fitting method to the data of photosphericmagnetic properties and solar flare magnitudes, and evaluated a simultaneous tolerance interval.Data samples are composed of 21 flares and 14 active regions. The solar flare magnitude is obtained from theGOES satellite 1-8 angstrom data. The largest and smallest flares in the sample are X17 (1.7 x 10^{-3} Wcm^{-2}) and A5 (5.0 x 10^{-8} W cm^{-2}), respectively. The photospheric magnetic properties are derivedfrom the vector magnetograms of the Solar Flare Telescope (Mitaka, Japan) and from the SoHO/MDImagnetograms. The photospheric magnetic properties are evaluated by using magnetic flux, magnetic fieldstrength, current density and others. We applied the linear fitting method to the data of the flare magnitudes andthe magnetic properties of the regions. In the linear fitting equation a probability and a confidence level are set,and then a simultaneous tolerance interval is obtained. If we use the magnetic field strength and the flare regionarea as magnetic parameters, a simultaneous tolerance interval is about a factor of 3.3 with 0.90 probability and0.90 confidence level.

- 83 -

SB42-2

Sensitivity of the Earth's Magnetosphere to Solar Wind Activity:Three-Dimensional Macroparticle ModelBaraka, Suleiman and Ben Jaffel, Lotfi

Institut d'Astrophysique de Paris, UPMC, CNRS, 98bis Blvd Arago, 75014,Paris, France

A new approach is proposed to study the sensitivity of the Earth's magnetosphere to the variability of the solarwind bulk velocity. The study was carried out using a three-dimensional electromagnetic particle-in-cell code,with the microphysics interaction processes described by Maxwell and Lorentz equations, respectively, for thefields and particles. Starting with a solar wind with zero interplanetary magnetic Field (IMF)impinging upon amagnetized Earth, the formation of the magnetospheric cavity and its elongation around the planet were modeledover time until a steady state structure of a magnetosphere was attained. The IMF was then added as a steadysouthward magnetic field. An impulsive disturbance was applied to the system by changing the bulk velocity ofthe solar wind tosimulate a decrease in the solar wind dynamic pressure, followed by its recovery, for both zeroand southward IMF. In response to an imposed drop in the solar wind drift velocity, a gap (air pocket) in theincoming solar wind plasma appeared moving toward Earth. The orientation of the cusps was highly affected bythe depression of the solar wind for all orientation of IMF. The magnetotail lobes flared out with zero IMF due tothe "air pocket" effect. With the nonzero IMF, as soon as the gap hit the initial shock of the steady magnetosphere,a reconnection between the Earth's magnetic field and the IMF was noticed at the dayside magnetopause. Duringthe expansion phase of the system, the outer boundary of the dayside magnetopause broke up in the absence of theIMF, yet it sustained its bullet shape when a southward IMF was included. The expansion/contraction of themagnetopause nose is almost linear in the absence of the IMF but evolves nonlinearly with a southward IMF. Thesystem recovered its initial state on the dayside soon after the impulsive disturbance was beyond Earth for bothcases of zero and nonzero IMF. Comparison with existing observations from Cluster and Interball-1 seems toconfirm many of our simulation results.

SB42-3

MHD-PIC Interlocked Simulation Model in Space Plasma: Application toCollisionless ShocksTooru Sugiyama and Kanya Kusano

The Earth Simulator Center, JAMSTEC, 3173-25 Showa-machi, Kanazawa-ku, Yokohama, Kanagawa, JAPAN

A new simulation model has been developed to understand the multi-scale coupling in space plasmas. In this newmodel, so-called "macro-micro interlocked simulation", Hall-MHD and Particle simulations (PIC or Hybrid) aresimultaneously performed, and the mutual interaction between them is handled self-consistently. The model cantreat MHD-scale dynamics including particle kinetic effects. Here we have applied this interlocked simulationmodel onto a particle acceleration process (Diffusive shock acceleration) around a collisionless shock. Hall-MHDsimulation covers the whole system, and, only in the shock transition region, particle simulation is embedded toincorporate the injection problem of the non-thermal particles by the process of the wave-particle interaction atshock. In this model, since the motion of acccelerated non-thermal particles are continuously calclulated eventhough they traverse between the particle region and the Hall-MHD region, any artifactitious boundary conditiondoes not need to be imposed to the particle simulation, and thus we can carry out the calculation for much longertime than the case that just a particle model is used as the previous studies. As a result of that, we have revealedthe detail evolution of the diffusive shock acceleration, in which the energy spectrum is getting harder than that inthe case of only the particle simulation is used.

- 84 -

SB42-4

Numerical Modeling of Solar WindEiji Asano, Takuma Matsumoto, and Kazunari Shibata

Kwasan Observatory, Kyoto University, 17 Ohmine-cho Kita Kazan, Yamashina-ku, Kyoto City, Kyoto, 607-8471, JAPAN

We construct a space weather model by connecting the different regions such as the solar corona, solar wind, andthe Earth, which are treated as one system. We simulated solar wind plus coronal mass ejections (CMEs) in aregion between 2 and 50 solar radii by using CIP-MOCCT method in order to investigate the effects by thepropergation of CME and solar wind. We assumed dipole magnetic field to be the initial stage and spheromakmagnetic field at the surface of 2 solar radii. We show the results of this simulation. This study becomes a basis ofnumerical space weather prediction.

SB42-5

The Magnetoshere-Ionosphere Compound Systems for Various Solar WindConditionsShigeru Fujita1 and Takashi Tanaka2

1. Meteorological College and JST, Japan2. Kyushu Univ. and JST, Japan

For the weather forecast, we have to understand the fundamental physical process of the atmosphere -- the generalcirculation. This situation holds for the space weather. Namely, we need to understand the fundamental physicalprocess for the global magnetosphere-ionosphere system. Therefore, it is essential to comprehend globalphenomena in the magnetosphere in terms of the magnetosphere-ionosphere compound system [Tanaka, 2003]. In the compound system, the Maxwell stress invoked by the reconnection between the solar wind magnetic fieldand the magnetospheric one drives the magnetospheric plasma convection. This magnetospheric convection isconnected with the ionospheric convection. Furthermore, the ionospheric convection is related to the ionosphericelectric current driven by the magnetospheric FAC. Bearing in mind that the magnetospheric current is driven byenergy converted from the thermal energy, the global self-consistency among the magnetospheric convection, theionospheric convection, the ionospheric current, the magnetospheric current, and the magnetospheric pressuredistribution holds in the magnetosphere-ionosphere compound system.The configuration of the compound system is controlled by the solar wind. It is instructive to investigatesystematically the configuration of the magnetosphere-ionosphere compound system. In particular, it isinteresting to consider the compound system for quite small IMF intensity. In this case, there is no reconnectionbetween the solar wind magnetic field and the magnetospheric one. Thus, no Maxwell stress drives themagnetospheric convection. However, our simulation indicates the magnetosphere-ionosphere convectionappears even in this condition. This convection seems to be driven the magnetosheath current that prevents themagnetospheric field from expanding across the magnetopause.

- 85 -

SB42-6

MHD Simulation of the Magnetic Storm Event for December 13-16, 2006R. Morishita, K. Mase, M. Amano, and T. Ogino

Solar-Terrestrial Environment Laboratory, Nagoya University, Japan

A three-dimensional global MHD simulation of interaction between the solar wind and the earth's magnetospherehas been executed to study the magnetic storm event on space weather problem for December 13-16, 2006, whenlarge interplanetary disturbances were generated in association with the strong solar activity of X-class flare.Characteristic features of the event are two X-class flares on 12/13 and 12/14 in the interval of rather quiet solaractivity, north-south fluctuation of IMF and a long duration of southward IMF from 12/14, arrival of a high speedsolar wind during the time for southward IMF. In the simulation, the high speed solar wind compresses themagnetosphere and magnetic reconnection occurs in the tail as long as at the dayside magnetopause for rapidsouthward turning of IMF from northward IMF and hot plasmas are injected around the geosynchronous orbitfrom the plasma sheet. During the interval when IMF By gradually changes from negative to positive, themagnitude of IMF extremely decreases to bring attenuation of magnetic reconnection. The open-closed boundaryshrinks in the polar cap and the transient expansion of the magnetic field lines occurs to imply enhancement ofparticle precipitation. The reconnection site moves from dawn to dusk in the dayside magnetopause and a plasmasheet is inclined and patchy and intermittent reconnection continuously happens in the tail.

- 86 -

SB51I-1

Mid-continent Magnetoseismic Chain (McMAC) and Its Role in FutureMagnetoseismic Research of Ultra Large Terrestrial InternationalMagnetometer Array (ULTIMA)Peter J. Chi1, Christopher T. Russell1, Mark B. Moldwin1, Mark J. Engebretson2, Ian R. Mann3, and Kiyohumi Yumoto4

1. Institute of Geophysics and Planetary Physics, University of California, Los Angeles, California, USA2. Physics Department, Augsburg College, Minneapolis, Minnesota, USA3. Department of Physics, University of Alberta, Edmonton, Alberta, Canada4. Space Environment Research Center, Kyushu University, Fukuoka, Japan

The Mid-continent Magnetoseismic Chain (McMaC) is a ground-based magnetometer project that focuses onmagnetoseismic research. McMAC consists of nine fluxgate magnetometer stations in the U.S. and Mexico alongthe 330th magnetic meridian. These McMAC stations are well aligned with the Fort Churchill Line of theCARISMA Array and two IGPP-LANL stations at the same longitude, forming a long magnetometer chain thathas the widest latitudinal coverage (29.7 to 78.6 deg cgm) at any single longitude on the Earth. In this paper wepresent the observations jointly made by McMAC, CARISMA and IGPP-LANL Arrays through the use of twomagnetoseismic methods. The normal-mode method measures the abundant signatures of field line resonance inthe dayside magnetosphere and converts the measurements to the equatorial plasma density. The travel-timetechnique detects the plasmapause location in the nightside by finding the discontinuity in Pi 2 arrival time acrossthe magnetometer chain. We also introduce the McMAC data products, such as the time series at multiplecadences, cross-phase and cross-power spectrograms, the fundamental mode frequencies, and the inferredequatorial mass densities. In the end we discuss our vision of the next logical step of magnetoseismic research inthe era of Ultra Large Terrestrial International Magnetometer Array (ULTIMA), including the magnetoseismicobservations at multiple longitudes, the comparison with numerical modeling results, and the coordination withother ground-based and space-based observations.

SB51I-2

MAGDAS Global Network and Its Data AvailabilityGeorge Maeda, Shuji Abe, Kiyohumi Yumoto, and MAGDAS Group

Space Environment Research Center, Kyushu University, Hakozaki, Fukuoka, Japan

We wish to present an update on the deployment of the MAGDAS global network, and also explain its dataavailability to the scientific community. SERC is nearing its completion of 50 realtime magnetometers deployedalong the 210 Magnetic Meridian and the dip equator. Each unit is sending geomagnetic ground datacontinuously (i.e., in near realtime) to a central server located at SERC. This data is available to you via theInternet. In addition, MAGDAS is a key member of ULTIMA, which was established one year ago to coordinatedata collection and exchange among all leading international magnetometer arrays.

- 87 -

SB51-1

Ultra Large Terrestrial International Magnetic Array (ULTIMA)Kiyohumi Yumoto1, Christopher T. Russell2, Brian J. Fraser3, Vassilis Angelopoulos4, Ian R. Mann5, and Peter J. Chi2

1. Space Environment Research Center, Kyushu University 6-10-1 Hakozaki, Higashi-ku, Fukuoka, Japan2. Institute of Geophysics and Planetary Physics,UCLA, Box 951567 Los Angeles, CA 90095-1567,USA3. Centre for Space Physics,University of Newcastle,University Drive, Callaghan NSW 2308, Australia4. Space Sciences Laboratory, University of California at Berkeley,Centennial Dr. at Grizzly Peak Blvd., CA 94720-7450,USA5. Faculty of Science , University of Alberta, 114 St - 89 Ave, Edmonton Alberta, T6G 2E1, Canada

The Ultra Large Terrestrial International Magnetic Array (ULTIMA) is a new international consortium that aimsat enhancing collaborative research and data exchange on the magnetosphere, ionosphere, and upper atmospherethrough the use of ground-based magnetic field observatories. ULTIMA is composed of individual magnetometerarrays in different countries/regions, and it provides a platform for each of them to easily and efficientlycollaborate with other arrays in order to expand observational coverage. ULTIMA also helps identify theimportance and need of individual arrays to continue operation or establish new stations in their host countries. Inthis paper we introduce the organization of ULTIMA and its observational coverage. We also describe the plansfor data exchange and distribution through individual data servers and virtual observatories, providingopportunities for the scientific community to access an unprecedented amount of integrated ground-basedmagnetometer observations for heliophysics research.

SB51-2

Ground Distributed Magnetometer Array Techniques for ULF and EMICWave StudiesSean T. Ables and Brian J. Fraser

Centre for Space Physics, School of Mathematical & Physical Sciences, University of Newcastle, Callaghan, NSW 2308Australia

Close-spaced magnetometer arrays located at high and low latitudes may be used to measure the phase andpropagation characteristics of ultra-low frequency (ULF) and electromagnetic ion cyclotron (EMIC) waves in themagnetosphere. ULF wave cross-phase techniques can be used to determine the mass-loaded ion density alongclosed field lines in the magnetosphere and locate the open-closed field line boundary at high latitudes. Phase andpolarisation techniques may also be used to determine the exit point of EMIC waves propagating down field linesinto the ionosphere. Examples will be presented that illustrate some important future applications that may beutilized by reasonably close-spaced ground magnetometer arrays.

- 88 -

SB51-3

CHAIN-project and Installation of the Flare Monitoring Telescope in PeruSatoru UeNo1, Kazunari Shibata1, Reizaburo Kitai1, Goichi Kimura1, Yoshikazu Nakatani1, Shin'ichi Nagata1, Ken'ichi Otsuji1, Jose K. Ishitsuka2, and Mutsumi Ishitsuka2

1. Kwasan and Hida Observatories, Kyoto University, Kamitakara, Takayama, Gifu 506-1314, JAPAN2. Instituto Geofisico del Peru, Etapa, Ate, Lima 3, PERU

The Flare Monitoring Telescope (FMT) was constructed in 1992 at Hida observatory in Japan to investigate thelong-term variation of solar activity and explosive events. It has been part of the international coordinatedobservations program (STEP) since 1991. It has five solar imaging telescopes that SIMULTANEOUSLY observethe full-disk Sun at different wavelengths around H-alpha absorption line or in different modes. Therefore, it canmeasure the 3 dimensional velocity field of erupting filaments on the full solar disk without the visual effect dueto the seeing. Moreover, it can detect Moreton-waves (shockwaves on the chromosphere) that accompany solarflares. These observations of physical properties of solar explosive phenomena play a very important role for thespace-weather research. We want to monitor a lot of solar flares and erupting filaments continuously as much aspossible by using several of such characteristic telescopes. Then, we have started to execute "Continuous H-alphaImaging Network (CHAIN)-project" as part of the CAWSES project. As part of CHAIN-project, we areexamining the possibility of installing of the telescopes in foreign countries. Then, we selected the campus of theIca University in Peru as the candidate-site where the 1st oversea FMT will be installed. Currently, we areinvestigating various items, aiming to start the operation of the FMT in Peru by the end of 2009 before the nextmaximum phase of solar cycle. In this meeting, we introduce the outline of our project and the investigations forinstalling the FMT in Peru.

SB51-4

One Solar Cycle Observation of Solar Activities by Flare MonitoringTelescope of Hida ObservatoryReizaburo Kitai, Miwako Katoda, Goichi Kimura, Yoshikazu Nakatani, Mai Kamobe, Satoru Ueno, and Kazunari Shibata

Kwasan and Hida Observatories, Kyoto University, Kamitakara, Takayama, Gifu, 506-1314, JAPAN

Since 1992, solar activities have been observed by Flare Monitoring Telescope (FMT) at Hida Observatory, KyotoUniversity. Full solar disk has been monitored in five wavelengths around H alpha line. The images have beenrecorded both in video format and in digital form. Active events have been checked visually by video movies,classified and compiled in our database, which is open to the world community. Thanks to multi-wavelengthobservation scheme of FMT, we can study detailed dynamics of H-alpha plasma in active phenomena. Severalscientific results, which is related to space weather, will be given in this report. (1) Dynamics of filamenteruption: Applying the cloud model analysis, 3-dim velocity fields of erupting gas were derived. It was confirmedthat all the high velocity eruptions were associated with CMEs. (2) Moreton wave: Around 30 Moreton waveswere detected by FMT. From case studies of wave events, it is found that Moreton waves are different from EITwaves. (3) Butterfly diagrams: Diagrams for strongly active events such as flares, filament eruptions and surges,are silimar to the sunspot diagram, while that of transient tiny-dark-points is different from the others. We thinkthat tiny-dark-points will be ephemeral active regions on the solar surface.

- 89 -

SB52I-1

Climatological Variations in the Ionosphere and Upper AtmosphereMartin J. Jarvis1, John T. Emmert2, and WG 4.43

1. British Antarctic Survey, Cambridge, UK, CB3 0ET2. E. O. Hulburt Center for Space Research, U.S. Naval Research Laboratory, Washington, D.C., USA3. CAWSES

Understanding the climatology of the ionosphere and upper atmosphere is prerequisite to identifyinganthropogenically-induced or naturally-occurring secular trends. In the upper atmosphere the huge impact of solarvariability means that a climatology must include not only the long-term mean but also the solar cycle andseasonal variations. Several climatologies have recently been published. However, to produce a climatologywhich covers as large an altitude range and spatial area as possible, data from a variety of observationaltechniques have to be used. As part of CAWSES WG 4.4 objectives, a survey of available data and techniques forthe neutral upper atmosphere has been undertaken and a similar survey for the ionised atmosphere is underway.Combined, these two surveys will summarize the climatological and long-term data needs of the scientificcommunity and point to future observational requirements.

SB52I-2

Access to Space Weather Data through the Virtual ObservatoriesRaymond J. Walker1, Jan Merka3, Todd A. King2, Steven P. Joy2, and Tom Narock3

1. Institute of Geophysics and Planetary Physics and Department of Earth and Space Sciences, UCLA, Los Angeles, CA9009501567, USA2. Institute of Geophysics and Planetary Physics, UCLA, Los Angeles, CA 90095-1567, USA3. Goddard Earth Sciences and Technology Center, University of Maryland, Baltimore, MD and Heliophysics ScienceDivision, NASA GSFC, USA

Space physics data are widely distributed. This can complicate space weather studies which can require data fromthe Sun to the ionosphere. Successful management of such distributed data repositories requires a combination ofexpertise in both science and information technology. The NASA Heliophysics Division has established a groupof discipline virtual observatories (VOs) to provide the scientific community with access to well documented dataand services. We will demonstrate the management of a distributed data system by using the example of theNASA Virtual Magnetospheric Observatory (VMO). The VMO creates robust links to the world's relevant databases thus providing one-stop shopping for the magnetospheric researcher seeking data. A joint effort of scientistsat the Goddard Space Flight Center and UCLA, the VMO uses existing and widely adopted technologies andprovides well organized views of diverse science holdings. Since data are very dynamic especially during theearly phases of a mission, the VMO design allows frequent and asynchronous updating. The VMO providesaccess to value-added services (e.g. to reformat, manipulate, analyze and display data) developed both locally andremotely. The registries for both data and services are designed to make it easy for suppliers to make theirresources available and update information. Resources are described by using the SPASE data model. We havecreated tools to enable data repositories to populate the registries and communicate with the VMO even if they useother data models. Scientists trained in data management are available to work with data suppliers.

- 90 -

SB52-1

Solar Cycle Variation of Interplanetary Drivers of Intense GeomagneticStormsE. Echer1, W. D. Gonzalez1, B. T. Tsurutani2, and A. L. C. Gonzalez1

1. Instituto Nacional de Pesquisas Espaciais (INPE), Av. Astronautas, 1758, Sao Jose Campos, SP, Brazil2. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA

Intense geomagnetic storms (Dst &#8804; -100 nT) occur when the solar wind-magnetosphere energy coupling isenhanced, through the magnetic reconnection mechanism. This occurs preferentially when the interplanetarymagnetic field (IMF) Bz component is southwardly directed (Bs- in GSM). The interplanetary sources of Bs fieldshave different interplanetary and solar origins. In this work, we identify the solar cycle dependence of theinterplanetary drivers of intense magnetic storms during solar cycle 23. We have found that the most importantstructures leading to intense Bs (and intense magnetic storms) are magnetic clouds (MC), sheath fields (Sh),combined sheath and MC fields (Sh+MC) and corotating interaction regions (CIRs). During the rising phase ofthe solar cycle, MCs are the dominant structure followed by sheath fields. At solar maximum, sheath fieldspredominate, followed by MC and then Sh+MC. During the declining phase, MCs and CIRs are the maininterplanetary structures leading to intense storms.

SB52-2

Tracking Intense Geomagnetic Storms to the Interplanetary Medium andSolar SourcesBrigitte Schmieder1, Sergio Dasso2, Christina Mandrini3, Hebe Cremades 4, Consuelo Cid5, Y. Cerrato5, E. Saiz5, Angela Aran6, Michel Menvielle7, Stefaan Poedts8, Luciano Rodriguez9, and Andrei Zhukov10

1. Observatoire de Paris, LESIA, Meudon 92195, France2. Instituto de Astronomia y Fisica del Espacio, CONICET-UBA, Buenos Aires, Argentina3. Departamento de Fisica, Facultad de Ciencias Exactas y Naturales, Universidad de4. NASA Goddard Space Flight Center, Greenbelt, MD, USA5. Universidad de Alcala, Madrid, Spain6. Universitat de Barcelona, Espana7. Centre d'etude des Environnements Terrestre et Planetaires, Velizy, France8. K.U. Leuven, Leuven, Belgium9. Solar Influences Data analysis Center, Royal Observatory of Belgium, Brussels,10. Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia

On May 15, 2005, at 02:38 UT an interplanetary shock was recorded by ACE. The following interplanetarystructure produced an important geomagnetic storm (minimal value of the Dst index -263 nT). Analysis ofinterplanetary (plasma and magnetic) observations has shown that these disturbances could correspond to thearrival of magnetic clouds.The main trigger of the geomagnetic storm is definitively the fast halo CME of May 13 (LASCO) observedconsequently to the flare occurring at 17:22 UT in the active region 10759. However, the analysis of thecomplexity of the magnetic cloud parameters (ACE) leads us to different possible scenarios for the interpretation,either the existence of two clouds produced by two different events on May 15 (different filament eruptions), orthe presence of only one complex cloud resulting from the main AR filament eruption.The helicity and the orientation of the CMEs and the magnetic clouds are compared in both cases.

- 91 -

SB52-3

The Probability Forecast of Geomagnetic Storm OccurrencesKen Tsubouchi

National Institute of Information and Communications Technology, Koganei, Tokyo 184-8795, Japan

We have evaluated the occurrence frequency of intense geomagnetic storms by analyzing the statistical propertiesof its waiting-time, the time interval of the successive events. Intense storms are characterized by their peak Dstless than -100 nT, and 322 events are obtained in the Dst-available period from 1957 to 2001. The distribution ofthe waiting-time exhibits a power-law tail in the range longer than 1000 hours, both for the solar active (an index= -2.2) and quiet phases (-1.4). Following the work of the solar flare statistics that the power-law distributionindicates the time-dependent Poisson process [Wheatland and Litvinenko, 2002], we assume that the interval ofstorm occurrences is also governed by a solar cycle-dependent Poisson process. The ordinary chi-square tests ofgoodness of fit practically accept this hypothesis. The mean occurrence rate (per three months) is 2.3 for the solaractive phase and 0.7 for the quiet phase. By giving the Poisson distribution based on these values, we try todevelop a scheme for forecasting the storm occurrence probability in a long-term range. The performance of theresults is verified by examining the Brier score, the conventional criterion for the weather probability forecast. Wewill further report how to build a model with higher accuracy.

SB52-4

Solar Activity Variation in Grand Solar Minima Deduced from CosmogenicRadiocarbonKimiaki Masuda1, Kentaro Nagaya1, Hiroko Miyahara2, and Toshio Nakamura3

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan2. Department of Earth & Planetary Science, University of Tokyo, SciBldg#1, 7-3-1 Hongo, Tokyo 113-0033, Japan3. Center for Chronological Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan

The sun is variable in its magnetic activity with various periodic cycles such as 11-year Schwabe cycle and longercycles. Solar activity variation affects the intensity of galactic cosmic rays entering earth's atmosphere andtherefore production rate of cosmogenic isotopes. Annual content of radiocarbon, which is one of cosmogenicisotopes, in tree rings reflects the change of cosmic ray intensity and therefore the solar activity. In the MaunderMinimum (1645-1715 AD), one of grand solar minima when sunspots were almost absent and the solar activitywas very weak, the cycle length of radiocarbon content was much longer than 11-year, indicating the solarSchwabe cycle was also longer. In the Spoerer Minimum (1416-1534 AD), which is considered to be anothergrand solar minimum, however, the cycle length was almost 11-year. In order to confirm whether the variabilityof cycle length in grand solar minima is related to the long term variation, we have measured annual radiocarboncontent in extended periods in the last 1200 years. Based on the result, we will discuss the difference in solar cyclelength for solar grand minima. Relation of the past solar activity and the global climate change will be alsomentioned.

- 92 -

P1-001

The Yoshimura Cycle in the Solar Magnetic Activity and Its Relation toClimate VariabilityVictor Velasco and Blanca Mendoza

Instituto de Geofisica, Universidad Nacional Autonoma de Mexico, Ciudad Universitaria, 04510, Mexico DF, Mexico

For the long time the sun has suspected to influence decade-to-century climate changes. The absence of long-termmeasurements of the climatic and solar activity phenomena has been one of the principal difficulties inquantifying the role of the sun in climate change.The influence of solar activity changes on climatic phenomena is currently debated. In this context, little attentionhas been given to the large scale climatic phenomena: the Northern Atlantic Oscillation (NAO), the AtlanticMultidecadal Oscillation (AMO), the Pacific decadal oscillation (PDO) and the Southern Oscillation Index(SOI).The nature of the climatic response to solar variability is assessed over a long-time scale. The waveletanalysis applied to paleoclimatic proxy data of large scale atmospheric phenomena (NOA, AMO, PDO and SOIIndex) has revealed coherence between the climatic oscillations and the solar phenomena (the cosmogenicisotopes) preferentially with period of Yoshimura cycle (60 yrs) that may reflect a modulation of solar activity.

P1-002

The Role of Deuterium as a Tracer of Solar-Climate RelationshipAlessandra Abe Pacini1, Ezequiel Echer1, and Heitor Evangelista2

1. Instituto Nacional de Pesquisas Espaciais (INPE), Departamento de Geof¡¦ica Espacial, S¡¦ JosêÂdos Campos, 12201 970,SP, Brasil.2. Laborat¡¦io de Radioecologia e Mudan¡¦s Globais (LARAMG), Universidade do Estado do Rio de Janeiro, Rio de Janeiro,20550-013 RJ, Brazil.

We present in this work an analysis of the role of deuterium as a tracer of Solar-Climate relationship. This studywas motivated by recent results of a ~100 year delta-D series, which showed a strong suggestion of thedependence between the delta-D time variability and the 11-year solar activity cycle. This correlation can not beexplained by the current models. Using the available experimental data (solar and isotopic), we test the hypothesisthat there is a nonprimordial deuterium flux created during solar flares, reaching the Earth and interacting with itsatmosphere, modulating some climatic parameters. The results obtained in this study represents a relevant contribution for the knowledge of the solar physical processes and terrestrial climatic condition relationships, andwill allow new interpretations about the local and global climatic variations occurred in the last century.

- 93 -

P1-003

Effect of Solar Activity on VHF Scintillations Observed at HyderabadDuring 2001-2004Yellaiah.Ganji and Nagasrinivas M.P

Department of Astronomy, Osmania University, Hyderabad - 500 007 (A.P), INDIA

Plasma instabilities in the nighttime F region of the equatorial ionosphere often give rise to irregularities in theplasma. Radio waves traversing the ionosphere from artificial satellite or radio stars experience a distortion inamplitude and phase due to these irregularities in the ionosphere. They vary widely with frequency of the wave,magnetic and solar activity, time of the day, latitude and propagation path geometry. The effect of fading andenhancement of amplitude about the median level, phase fluctuation and variation in angle of arrival are termedscintillations.VHF Scintillations have been studied by measuring the variations in the amplitude of FLEETSAT signal at 250MHz over Hyderabad (17.2deg N; 78.3deg E). These studies show that the occurrence of scintillations is moreduring pre-mid night hours than post midnight hours. The observations of VHF scintillations show that activityduring the year 2001-02

P1-004

Cosmic Ray Induced Ionization: A Full Physical ModelIlya G. Usoskin1 and Gennady A. Kovaltsov2

1. Sodankyla Geophysical Observatory (Oulu unit), POB 3000, FIN-90014 University of Oulu, Finland2. Ioffe Physical-Technical Institute, St. Petersburg, Russia

Cosmic rays play an important role in the terrestrial environment affecting physical-chemical properties of theatmosphere. Here we present a detailed model of the cosmic ray induced ionization (CRII) developed in theframeworks of CAWSES (CAWSES News, v.3, #2, p.6-7). The model (Usoskin and Kovaltsov, JGR, 111,D21206, 2006) is based on the Monte-Carlo CORSIKA+FLUKA tool, which simulates full development of anelectromagnetic-muon-nucleonic cascade in the atmosphere. The model is applicable to the entire atmosphere,from the ground up to the stratosphere. A comparison to fragmentary direct measurements of the ionization in theatmosphere confirms the validity of the model in the whole range of geographical latitudes and altitudes. Thisprovides a new tool for a quantitative study of the space weather influence upon the Earth's environment. Here we present an overview of quantitative effects of CR modulation on different time scales. Short transientphenomena (hours-days) have a minor global effect but may become significant in polar regions and highaltitudes. The effect of the 11-year cyclic variation is most pronounced globally. CRII regional effects of thegeomagnetic field changes become notable on time scales longer than a century. In particular, regional effects ofthe migration of the geo-magnetic dipole axis may overcome global changes due to solar activity variations insome mid-latiude regions.

- 94 -

P1-005

Solar Signal in the Monsoon and Post Monsoon Total Precipitable Waterover Peninsular India RegionRajesh J. and K. Mohankumar

Department of Atmospheric Sciences, Cochin University of Science and Technology, Cochin , India .

The present study uses monthly specific humidity from NCEP/NCAR for a time period of 55 years from1950-2004. Total precipitable water (TPW) was computed between 1000-850, 850-700, 700-600 and 600-500hPa. TPW was then averaged spatially between 74-78 E and 7-14 N and temporally for the monsoon and postmonsoon seasons. It was subjected to wavelet analysis. During the monsoon season TPW in the layer from1000-700 hPa shows 10-12 year oscillations, which is significant at 5% level. In the global wavelet spectrum thisfalls below 5% level still significant at 10%. For post monsoon season the wavelet spectra showed 10-12 yearvariability significant at 5% level for TPW between 1000-850, 850-700 and 700-600. The spectrum for 600-500hPa TPW shows 10-12 year mode at 90% significance only.The correlation between monthly values of 10.7 cm solar radio flux and tropospheric air temperature was studiedalong vertical sections along 80 E and 10 N. The cross-section along 80 E shows that in the northern hemispherethe correlation extends down to about 850 hPa up to 15 N and is significant at 1% level. High correlation extendsfurther north to 25 N and down to 950-hPa level but with less significance. Cross section at 10 N shows that thecorrelations are significant down to 800 hPa in the eastern hemisphere. It is suggested that the influence of solarflux on the tropospheric temperature, though feeble but statistically significant, may be driving the decadal modein the moisture.

P1-006

The Role of Solar and Geomagnetic Activity in Terrestrial Climate ChangeGely A. Zherebtsov, Vladimir A. Kovalenko, and Sergey I. Molodykh

Institute of Solar-Terrestrial Physics SB RAS, Irkursk, Russia

A possible contribution of solar activity effect to the global warming observed in the 20th century is discussed.The principal cause that casts some doubt upon the real significance of the solar activity effect on weather andclimate implies that in all climatic models the solar activity effect is generated by the direct action (solar radiationvariation) upon the troposphere which can not significantly influence on the terrestrial climate change. A new conception is presented of the solar activity effect on terrestrial climatic system parameters controlling theenergy flux that goes from the Earth to outer space in high-latitude regions. Physical mechanism of the solaractivity influence on high-latitude troposphere parameters is discussed. A connecting-link between solar activityand troposphere climatic characteristics is atmosphere electricity. The main factor that influences weather-climaticcharacteristics of the troposphere is parameters of the solar wind and interplanetary magnetic field whichdetermine geomagnetic activity and, correspondingly, the ionosphere-Earth electric potential in polar regions.Invasion of intense solar cosmic-ray fluxes, generated during solar flares, also exerts significant effect on thehigh-latitude troposphere electric field. The troposphere electric field has a great impact on the distribution ofcharged aerosol along the altitude and hence on cloudiness formation conditions and radiation cooling of thehigh-latitude troposphere. Change in radiation balance of terrestrial high-latitude regions results in restructuring ofthe troposphere thermobaric field and in changes of circulation and temperature meridional gradient that definesheat transfer by meridian. As a result heat content of the terrestrial climatic system and the global climate change. Results of the analysis for the response of troposphere thermobaric characteristics to isolated heliogeophysicaldisturbances as well as regularities of space-time variations in the troposphere temperature are presented anddiscussed within the framework of the model under consideration and from observational data. A scenario for possible contribution of the solar activity to the observable troposphere temperature variations and

- 95 -

climatic changes in the 20th century is discussed in the context of the model considered. The model presented andthe analysis results allow us to conclude that the solar activity contributes essentially to the change of the heatcontent of the Earth's climatic system as well as to entire climate in the 20th century.

P1-007

Indirectly Correlating Solar Activity and GPS Derived AtmosphericPrecipitable Water Vapour During Storms Event at AntarcticaWayan Suparta1, Mohd. Alauddin Mohd. Ali1, Baharudin Yatim2, Norbahiah Misran1, and Grahame J. Fraser3

1. Department of Electrical, Electronic and System Engineering, Faculty of Engineering, Universiti Kebangsaan Malaysia,43600 Bangi, Selangor Darul Ehsan2. Institute of Space Science (ANGKASA), Universiti Kebangsaan Malaysia, 43600 Bangi, Selangor Darul Ehsan, Malaysia3. Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand

It is well known that the Sun is the driver of Earth's climate. However, the direct influence of solar activity onclimate change and in their physical mechanisms is still an open question and has proved difficult to answer.Recent solar-climate studies based on long-term data have shown correlations with high statistical significancebetween solar variability and global surface temperature and many of these studies are focused at mid-latituderegions. This paper presents a new method of determining and quantifying the solar influence on atmosphericprecipitable water vapour (PWV) for two cases of major geomagnetic storms, of November 2004 and May 2005.Scott Base (SBA), McMurdo (MCM4), Davis (DAV1) and Syowa (SYOG) stations in Antarctica were taken asthe observation sites. In the proposed method, the solar influence on PWV is determined indirectly by correlatingthe GPS PWV and total electron content (TEC) variations on a time-basis. In this work, TEC, which describes theintegrated ionospheric variability, is used as a solar activity parameter. The GPS PWV is extracted from zenithtropospheric delay (ZTD) which is determined from GPS signals and surface meteorological measurements, andTEC measurements are taken from different GPS satellites observed at arbitrary elevation angles which has thecapability to remove the instrumental biases both from the receiver and the satellites. Further to show clearly solarassociated event influence on PWV, two years data over the period of 2004-2005 from four sites above are alsoprocessed and analyzed. The results show a good significant correlation between PWV and TEC. It is also foundthat a clear seasonal signal is present, highest during summer and lowest during winter for both TEC and PWV inmonthly analyses. The challenge of these studies will be to develop new observing technologies that can fill

- 96 -

existing gaps at lower cost than current observational technologies, such as Radiosondes and water vapourradiometers (WVRs), and to improve the amount of available PWV information than is currently available due tolack of precise and continuous water vapour data at Antarctica.

P1-008

Long-term Regularities in Distribution of Global Solar and InterplanetaryMagnetic Fields.Pavel Ambroz

Astronomical Institute of the Acad. Sci. of the Czech Republic, 25165 Ondrejov, Czech Republic

Close relationship between distributions of the dipole component of global solar magnetic field and interplanetarymagnetic sector structure is investigated during last three solar activity cycles. Distribution of the patternsrepresenting both magnetic polarities from solar photosphere, on a source surface in solar corona and ininterplanetary magnetic field near the Earth orbit is followed during about 30 years long time period. Thevariation in the recurrence period during different phase of the activity cycle is found and the relationship betweennew active regions with strong magnetic flux emergence, large-scale transport of background magnetic regionsand global magnetic structures with low resolution spherical modes is studied in detail. Local magnetic regionoccurrences in photosphere are subordinate to rules leading to formation of global regularities observed ininterplanetary magnetic field near Earth orbit.

- 97 -

P1-009

A Challenge for Reconstruction of Solar Spectral Irradiance at the Top ofEarth's Atmosphere Using Ca-K Full-Sun ImagesMasaki Yokoyama and Satoshi Masuda

Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Japan

The final goal of this study is to reconstruct solar spectral irradiance for 100 years from the beginning of the lastcentury using full-sun image data derived from ground-based observations. The aims of our study toward this goalare to connect between solar surface conditions seen in full-sun image data and solar spectral irradiance variations,and to estimate solar spectral irradiance from ground-based solar image data with difference of 2% or less. Weused Ca-K full-sun image data taken at the BBSO and solar spectral irradiance data measured by the SORCEsatellite. For reconstruction of solar spectral irradiance, we employed a simple model that solar spectral irradianceis composed of three components (dark region, quiet region and bright region), and we evaluated spectralirradiance of each component from July 2004 data. We compared our reconstruction and observational datameasured in August 2004. The difference between them was less than 2% in the wavelength range from 200 to1600 nm and less than 9% in the wavelength range from 116 to 200 nm. This model is good for longerwavelengths than 200 nm, but not accurate enough for shorter wavelengths than 200 nm. Solar radiation of shorterwavelengths than 200 nm is characterized by strong emissions originated from the transition region. So, our modelrequires improvements for evaluating these emissions in order to reconstruct solar spectral irradiance with a highaccuracy.

P1-010

Ionospheric and Geomagnetic Response to Changes in IMFSubhash C. Kaushik1, Ashutosh Shrivastava2, Kamal Agarwal2, Hari Mohan Rajput2, and Sonia Sharma2

1. Department of Physics, Government Autonomous Post Graduate College, Datia, M.P. 475 661, India.2. School of Studies in Physics, Jiwaji University, Gwalior, M.P., India.

During the daily variations of the F region electron density distribution greatly affects the propagation of radiowaves through the ionosphere. The Interplanetary Magnetic Field (IMF) has been found to play a very importantrole in the solar- terrestrial relationship. Investigators have revealed that three features of IMF, namely the IMFsector boundary crossings, the variability of the north- south (BZ) component and the polarity reversals of radial(BX) or azimuthal (BY) component, have great influence on Sun - Weather relationship, geomagnetic phenomenaand many other ionospheric phenomena including the E and F region drifts. Further the magnetic cloud events(MCEs) being the manifestation of the coronal mass ejections (CMEs) are found responsible for initiating largeand intense geomagnetic storms. In this paper we describe these magnetic cloud events and intense geomagneticstorms recorded by various geomagnetic observatories with Dst values >= -300 nT. We further discuss the effectsof these intense geomagnetic storms on near Earth space. During storm phase, which definitely indicates thepresence of the sheath region existing ahead of a magnetic cloud. In this work we used hourly values of IMF dataobtained from the NSSD Center. The analysis mainly based on looking into the effects of BZ and B values. TheIMF on the E and F region mid day (10-14 hours) and mid night (2200-0200 hours). The high-resolution data IMFBZ and solar wind data obtained from IMP-8 satellite was available during the selected period. The interplanetaryelectric field in the east west direction (EYY) is calculated as EYY = VSW * BZ . The data is separated in todifferent sets corresponding to (i) northward IMF (passage of positive magnetic clouds), (ii) southward IMF (thepassage of negative magnetic clouds), (iii) day time, (iv) night time and their combination to study the relationbetween interplanetary electric field and equatorial ionospheric electric field at various background conditions.From the various results published on the effects of these events on ionosphere and magnetosphere and the

- 98 -

observations presented here at equatorial and low latitudes, it is reported here that during the great magneticstorms sufficiently large magnetospheric electric fields are produced that penetrate to low and equatorial latitudesdue to insufficiently shielding by space charge at inner edge of plasma sheet. Both penetrating magnetosphericelectric field and electric field generated by ionospheric disturbance dynamo (IDD) further produce unusualionospheric electric field electron density irregularities. Both AP and AE show rise before the forward turningswhile the Dst index shows a classic storm time decrease. The analysis indicates that the magnitude of all theresponses depends on BZ component of IMF.

P1-011

The Northern Annular Mode in Summer and Its Relation to Solar ActivityVariations in the GISS ModelEJae N. Lee1, Sultan Hameed1, and Drew T. Shindell2

1. Institute for Terrestrial and Planetary Atmospheres, Stony Brook University, Stony Brook, NY 11794-5000, USA2. NASA Goddard Institute for Space Studies and Columbia University, USA

The Northern Annular Mode (NAM) has been successfully used in several studies to understand the variability ofthe winter atmosphere and its modulation by solar activity. The variability of summer circulation can also bedescribed by the leading Empirical Orthogonal Function (EOF) of geopotential heights. We compare the annularmodes of the summer geopotential heights in the northern hemisphere stratosphere and troposphere in theGoddard Institute for Space Studies (GISS) ModelE with those in the National Centers for EnvironmentalPrediction/National Center for Atmospheric Research (NCEP/NCAR) reanalysis. In the stratosphere, the summer NAM patterns in both model and observation are consistent with the interpretationthat low NAM conditions represent an enhancement of the seasonal difference between the summer and theannual averages of geopotential height, temperature and velocity distributions, while the reverse holds for highNAM conditions. Composite analysis suggests that the summer stratosphere is more "summer-like" in the solarmaximum. This means that the zonal easterly wind flow is stronger and the temperature is higher than normal. Thus increased irradiance favors a low summer NAM. A quantitative comparison of the anti-correlation betweenthe NAM and the solar forcing shows that the increased irradiance favors a low summer NAM. The temperaturefluctuations in simulated solar minimum conditions are greater than in solar maximum throughout the summerstratosphere.The summer NAM in the troposphere obtained from both the observation and the GCM has a dipolar zonalstructure with maximum variability over the Asian monsoon region, though the results are not statisticallysignificant.

- 99 -

P1-012

Stastical Analysis on the Association of Photospheric Cancellations andFilament Formations on the SunYusuke Iida and Takaaki Yokoyama

Department of Earth and Planary Science , University of Tokyo, Hongo , Bunkyo-ku , Tokyo , Japan

We statistically examined the association of cancellations of the photospheric magnetic fields and formations ofH-alpha filaments. Examples of such simultaneous occurrence were already reported and some theoretical modelsbased on such associations were proposed, which are divided into two categories, namely the flux emergingmodels and the reconnection models. However, there were few systematic studies on the association. So westatistically examined by using the full-disk H-alpha images taken by SMART, Hida Observatory, KyotoUniversity and the full-disk photospheric magnetograms of SOHO/MDI. We examined 7 active filaments and 10quiescent filaments from August to October in 2005. The results were as follows:(1)In active regions, there are 14cancellations without formations, 6 formations without cancellation, and 5 events. (2)In quiet regions, there are 19cancellations without formation, 13 formations without cancellations, and 2 simultaneous cancellations andformations. In both active and quiet regions, we observed filament formations without cancellations. But thefraction of formations without cancellations in quiet regions was more than that in active regions. From theresults, we discuss the difference of filament formation in active regions and quiet regions.

P1-013

Characteristics of Diurnal Variation in Indonesian Maritime ContinentBased on Wind Profiler ObservationsY. Tabata1, T. H. Seto1, H. Hashiguchi1, M. K. Yamamoto1, Y. Umemoto1, T. Shimomai2, Y. Shibagaki3, M. D. Yamanaka4, S. Mori4, F. Syamsudin5, and T. Manik6

1. RISH, Kyoto University, Japan2. Shimane University, Japan3. Osaka Electro-Communication University, Japan4. IORGC, JAMSTEC, Japan5. BPPT, Indonesia6. LAPAN, Indonesia

Indonesian Maritime Continent (IMC) is one of the most active convection areas in the world. Super CloudCluster (SCC), which appears in Indian Ocean and moves eastward, with Intraseasonal variation is modulated byactive convection with diurnal variation over IMC. However, the studies in IMC are insufficient because of thelack of observational data except for Sumatera Island.We installed Wind Profiler Radars (WPRs) at Pontianak and Biak in this year under the HARIMAU(Hydrometeorological ARray for ISV-Monsoon AUtomonitoring) project. We have already conducted continuousobservations since 22 February and 11 March, respectively. We plan to install another WPR at Manado in nextyear. In this study, we use WPR data, NCEP reanalysis wind velocity data, and blackbody brightness temperature (Tbb)data by GMS satellite. We can continuously obtain wind profiles below about 4 km. At the beginning of thisstudy, we compared WPR horizontal wind velocity with that of NCEP reanalysis, and have obtained consistentresults. In the analysis of Pontianak WPR data, we found that boundary layer development reaches 1.5 km from12 LT to 14 LT. Strong south-west wind exists from 0 LT to 6 LT. On the other hand, we found from Tbb datathat convection field appears near south-west coast of Borneo island around 14 LT, and it moves north-east.

- 100 -

Strong south-west wind can be explained as the flow to the convection field.In this presentation, we will also show the comparison among observation results at Pontianak, Biak, andKototabang.

P1-014

Quasi-biennial Oscillation in Geomagnetic Sq Ranges at Equatorial and LowLatitudesSandeep Kumar Bhardwaj

Indian Institute of Geomagnetism, New Panvel (W), Navi Mumbai 410 218, India

Monthly mean hourly values of geomagnetic field components D, H and Z for quiet days at equatorial and lowlatitude stations are analyzed to study the presence of Quasi-biennial oscillation (QBO) in Sq ranges. The dataused in this analysis is from 1958 to 1993 at equatorial electrojet stations: Trivandrum, Kodaikanal,Annamalainagar and from 1927 to 1997 at low latitude station Alibag. From this basic data, geomagnetic Sqranges and summed ranges are computed and subjected to the data adaptive, noise reducing technique of SingularSpectrum Analysis (SSA). A QBO like signal with a quasi-periodicity of ~ 24-month is detected in Sq rangespectrum. The pair of eigen vectors analyzed through SSA up to order 18 represent different oscillations of thefield such as; 11-year, annual, semi-annual, 4-month, 14-month (Pole-tide) and a quasi-biennial oscillation etc. The Sq ranges, summed ranges at all the stations and monthly mean sunspot numbers for the same period are alsoanalyzed by band pass digital filter to identify the source of QBO. It is found that a QBO signal with varyingamplitude (period 24 to 26-months) occurs in all the three ranges and summed ranges of D, H and Z and also inthe monthly mean sunspot numbers. The amplitude of the signal is stronger at equatorial electrojet stations incomparison with low latitude station Alibag and may be due to solar origin.

- 101 -

P1-015

Plasma Environment and Spacecraft Charging in Geosynchronous Orbit:Analysis and ForecastMasao Nakamura

Department of Aerospace Engineering, Osaka Prefecture University, Sakai, Osaka, 599-8531 Japan

Plasma environment in geosynchronous earth orbit (GEO) is closely related to spacecraft charging, that wouldcause spacecraft anomalies with induced electrostatic discharging (ESD). Intense fluxes of hot electrons withenergy in the range of several to several tens of keV, injected from the geomagnetotail into GEO between nightand morning local time during magnetospheric substorms, are mainly responsible for spacecraft surface charging.On the other hand, it is rare but not negligible that the electron sudden density enhancements with temperature ofa few to several keV in the pre-noon sector also cause spacecraft surface charging. We will discuss thesehazardous GEO plasma conditions and recent efforts to predict the variation of the GEO plasma environment forspacecraft charging forecast.

P1-016

The 11-year Solar Signal in Tropospheric Variability - a Model StudyAnne Kubin and Ulrike Langematz

Freie Universitaet Berlin, Berlin, Germany

We present a model study to show the tropospheric response to the 11-year solar signal. We conducted 11-yearsolar maximum and minimum experiments using the ECHAM5/MESSy climate model system. The extendedradiation code FUBrad was included enabling the model to better represent UV changes associated with the solarcycle. Spectral irradiance and solar cycle induced ozone changes were prescribed. The model was used in theT42L39 resolution to perform a 25-year solar minimum and maximum equilibrium simulation, respectively. Themodel simulates an improved poleward-downward movement of zonal wind anomalies during northern winter.We will discuss the tropospheric response to solar variability in terms of changes in the dominant modes ofvariability, such as the Arctic O scillation (AO) and the North Atlantic Oscillation (NAO). In the 25-yearsimulation we find an AO-like response pattern in January which extends from the stratosphere to the troposphereleading to near-surface changes in temperature and circulation during northern winter. To test the robustness ofthe results the simulations were extended to 50 years each.

- 102 -

P1-017

Quiet Sun Magnetism and IrradianceIballa Cabello and Vicente Domingo

Grupo de Astronomia y Ciencias del Espacio, Instituto de Ciencia de los Materiales, Universidad de Valencia, 46980 Paterna,Spain

We study the solar atmosphere structure around small magnetic elements present in the very quiet photosphere,away from active regions. Their radiative properties are described with a simple model based on data obtained atthe Swedish Solar Telescope at La Palma (G-band and CaII), ultraviolet and visible images obtained by TRACE,magnetograms by the Michelson Doppler Imager on SOHO, and diverse data by HINODE. The significance ofthe quiet sun small magnetic elements contribution to the total solar irradiance and its variations is considered.

P1-018

30-Day Variation of Global Lightning Activities and Its Relationship toTropical Cloud CoverageMitsuteru Sato1, Yukihiro Takahashi2, Yoshitaka Okazaki2, Hiroko Miyahara3, and Kazuyo Sakanoi4

1. Computational Astrophysics Lab., RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan2. Department of Geophysics, Tohoku University, Aramaki, Aoba, Sendai, Miyagi 980-8578, Japan3. University of Tokyo, Japan4. Komazawa University, Japan

In order to study the characteristics of the periodic changes of global lightning activities and to identify therelationship between global lightning activities and the tropical cloud coverage, we have analyzed ELF magneticfield waveform data obtained at Syowa station in Antarctica, Onagawa observatory in Japan and Esrange inSweden for the period between February 2000 and December 2004. We have estimated day-to-day variation ofthe Schumann resonance (SR) spectral intensity, which is the proxy of the global lightning activity, and havecalculated the power spectra of the SR spectral intensity variations using the maximum entropy method. Thepower spectra showed steep spectral peak at ~28-day in the solar maximum, which is comparable to the solarrotation period. On the other hand, in the solar minimum the power spectra showed steep spectral peaks at~35-day and ~15-day. These spectral characteristics are fairly consistent with those of the tropical cloud coveragevariations derived from the outgoing longwave radiation (OLR) data (Okazaki et al., 2007). We have alsoanalyzed the global IR cloud image data obtained by the meteorological satellites and have estimated the variationof the >8 km cloud coverage in the tropics. From a cross-spectral analysis between the cloud coverage variationand the SR spectral power variation, it is found that the phase distribution peaks at +/-180 deg at around ~30-dayperiod. This fact implies that the tropical cloud coverage has a negative feedback on global lightning activity.

- 103 -

P1-019

Investigation of Magnetic Reconnection in Two-Ribbon FlaresY.-H. Yang1, C. Z. Cheng1, S. Krucker2, and R. P. Lin2

1. Plasma and Space Science Center, National Cheng Kung University, Taiwan2. Space Sciences Laboratory, University of California, USA

It is generally believed that the energy release and particle acceleration in solar flares are associated with themagnetic reconnection in the corona. But the trigger mechanism of magnetic reconnection is still unclear. Sincethe reconnection is difficult to observe directly, investigation of the apparent motions of related chromosphericsignature, such as the hard X-ray (HXR) kernels or H-alpha ribbons, provides an important way to understand themagnetic reconnection process. Two physical quantities, reconnection electric field and magnetic flux change rate,are estimated in this study by using MDI (Michelson Doppler Imager) magnetograms, reconstructed HXR imagesfrom RHESSI (Reuven Ramaty High Energy Solar Spectroscopic Image), and H-alpha images from globalhigh-resolution H-alpha network. The characteristics of X- and M-class flares have been analyzed. Comparison ofreconnection rate between observation and theory will be discussed.

P1-020

Influence of Large Scale Variations in Convective Available PotentialEnergy (CAPE) and Solar Cycle on Temperature at Tropopause Regionover IndiaVivek Panwar1, S. K. Dhaka1, H.-Y. Chun2, Rupali Sapra1, T. K. Mandal3, and A. R. Jain3

1. Radio and Atmospheric Physics Lab, Department of Physics, Rajdhani College, University of Delhi, Delhi, India2. Department of Atmospheric Science, Yonsei University, Seoul, South Korea3. Radio and Atmospheric Science Division, National Physical Laboratory, New Delhi 110012, India

We have shown influence of large scale variation in convective available potential energy (CAPE) and solar cycleover temperature variation at 100 mb pressure level using daily radiosonde at 1200 Hrs GMT from 1989 to 2005over Indian region. Particularly results are striking at Delhi (28.30N, 77.10 E) and Kolkata (22.30 N, 88.20E).Both in CAPE and temperature, solar-induced signature with overriding dominant annual variations isinvestigated. CAPE itself modulated by solar cycle; however it has shown a control over the trends of temperaturein the tropopause region. Interestingly, the annual peak values of CAPE enhanced at Delhi during low solaractive period (1994-1997) occurring simultaneously with coldest temperature (-78 degree C) annual peaks at 100mb. No clear linear trends emerged in CAPE and temperature data at Delhi. However, at Kolkata, which is locatedfacing Bay of Bengal, there is a clear trend of decreasing temperature at 100 mb with rising trend in CAPE. Thedecrease in temperature is about 1.5 degree C in 17 years. Analysis suggests that trend of increasing convectiveactivity in the troposphere, at least partly, can leads to cooling trend in the tropopause region. Partly such variationmay be attributed to solar control depending on location.

- 104 -

P1-021

Variability of the Meridional Flow Profile with the Solar CycleUrmila Mitra-Kraev

University of Sheffield, Department of Applied Mathematics, Hicks Building, Sheffield S3 7RH, UK

Measurements of the solar meridional flow are very important as input for solar dynamo models and for activitycycle forecasts. We present meridional flow measurements of the Sun using a novel helioseismic technique toanalyze SOHO/MDI data in order to determine radial and temporal dependencies during solar cycle 23. Theresults show variability on various time-scales as well as variations with depth, indicating the development ofmultiple circulation cells previously found in numerical simulations.

P1-022

Interpretation of Physical Factors Responsible for Global and RegionalClimatic Responses to Long-Term Solar Activity VariationsOleg Raspopov1, Valentin Dergachev2, Olga Kozyreva3, Taneli Kolstrom4, and Evgeny Lopatin5

1. SPbF IZMIRAN, P.O. Box 188, 191023 St.-Petersburg, Russia2. Ioffe Physico-Technical Institute of RAS, St.-Petersburg, Russia3. Institute of Physics of the Earth, RAS, Moscow, Russia4. Merrijarvi Research Station, University of Joensuu, Finland5. Biology Institute of Komi SC of Ural Branch, RAS, Syktyvkar, Russia

Results of analysis of the climatic response to the quasi-two-hundred-year solar activity cycle (deVries cycle)based on generalized data on temperature variations in the Northern hemisphere and data on changes in climateparameters in six regions of the Northern hemisphere, i.e., Western Canada, Greenland, Spitzbergen, NorthernScandinavia, Tibetan Plateau, Tien Shan region in Central Asia, for the last 1000 years are presented. The resultsobtained indicate that the reconstructed temperatures in the Northern hemisphere (Briffa et al., 2000; Esper et al.,2002; Jones et al., 1998; Mann et al., 1999) point to a pronounced climatic response to solar forcing. This suggeststhat the climatic response to ~200-year solar activity variations has, on the whole, a global nature. Analysis for theregions of the Northern hemisphere mentioned above has revealed that Western Canada, Greenland, Tibetanplateau and Tien Shan are characterized by a distinct climatic response to solar forcing. At the same time, theresponse in the North Atlantic region (Spitzbergen and Northern Scandinavia) is weaker and manifests itself onlyin the second half of the last millennium. The results can be interpreted in the framework of the nonlinearresponse of the atmosphere-ocean system to the global influence of long-term solar irradiance variations. Indeed,as evidence by computer simulation, the regions of Central Asia and Western Canada are in the zones of a distinctpositive temperature response to external solar forcing, and Greenland is in the zone of a distinct negativetemperature response to external solar forcing. In its turn, the North Atlantic region is in the boundary zonebetween positive and negative climatic responses to solar forcing, which leads to weakening of the response and

- 105 -

even to zero response. Thus, in spite of a global nature of the climatic response to long-term solar activityvariations, it has a regional structure.

P1-023

Study of Equatorial Spread F Irregularities at Indian Low Latitudes UsingVLH and L-BandMalini Aggarwal1, H. P. Joshi1, K. N. Iyer1, A. K. Patra2, and Smitha V. Thampi3

1. Department of Physics, Saurashtra University, Rajkot2. National Atmospheric Research Laboratory, Gadanki, Tirupati3. Space physics laboratory,Vikram Sarabhai Space Centre, Trivandrum

Global positioning System (GPS) is a satellite based navigation system. The GPS radio signals are affected by theionosphere. The advent and evolution of GPS, and also the creation on its basis of widely branched networks ofGPS stations has opened up a new era in remote ionospheric sensing (Klobuchar, 1987). By using two frequencies(L1= 1575.42MHz and L2= 1227.6MHz) in GPS signals, it is possible to measure the ionospheric total electroncontent, TEC and Scintillation index S4. An important component of ionospheric plasma irregularity studies in theIndian low latitudes involves the study of the plasma bubbles which produce intense scintillations of thetransionospheric satellite signals. In order to investigate the dynamics of plasma density irregularities of differentscale sizes, a campaign of observations was conducted during 11 to 15 September 2005 at Gadanki(geog.13.450N, 79.170E, geomag. Coor. 4.440N, 151.730E), an Indian station. A low latitude spread F eventoccurred over India during the campaign on the night of 15 September 2005. The observations using dualfrequency GPS receiver, VHF coherent backscatter radar, and two ionosondes with some latitudinal separationhave been made. Range type spread F on ionograms and radar plume signatures on range-time-intensity maps ofthe VHF radar on the same day was also observed. Using the GPS receiver, the association of the fluctuations inthe intensity (S4 ~ 0.36 and 0.39) with the depletions in total electron content ( 5 and 12 TECU) are seen on thesame day which affect the positional accuracy of the GPS by 0.8m and 1.92m. The results of subsequentcampaigns will also be discussed.

- 106 -

P1-024

Long Term Comparative Study of Solar Wind and IMF Parameters withDst.Vidyacharan Dwivedi, Dr. C.M. Tiwari, and Dr. D.P. Tiwari

Department of Physics, A.P.S. University, Rewa (M.P.), 486003 , India

We have studied the long-term variation of solar wind plasma, interplanetary magnetic field (IMF) and sunspotnumber (Rz), with equatorial disturbance storm time Index (Dst), covering almost four solar cycle ( 21, 22 & 23).We found that 60% of the geomagnetic storms have occurred during the maximum phase of the solar activity. Ithas also been found statistically that the solar wind speed and Dst Index is highly correlated as compared to Dstand average value of IMF B, or Dst and Bz > 0, or Bz < 0. Moreover we find that 70% of the large geomagneticstorms are associated with southward component (Bz). Furthermore it is observed that the product of V and Bplays very significant role in occurrence of large geomagnetic storms. Significant differences are not observedfrom one cycle to another, inspite of the fact that the magnitude and profile of Rz is quite different in the fourcycles considered for our study. These results will also be discussed on the basis of other experimental/theoreticalfindings.

P1-025

Empirical Model of the High-Latitude Potentials During Storm TimesSatoshi Taguchi and Minako Morimoto

University of Electro-Communications, Tokyo 182-8585, Japan

Recent studies have shown that the cross polar cap potential drop in the ionosphere reaches more than 250 kVduring the superstorm while it saturates. Since the period of such extreme situations is rare, the potentialdistribution over the entire high-latitude ionosphere is difficult to obtain only from observations. In fact, oursurvey of DE-2 electric field data from more than 2000 passes has shown that it is only for the IMF magnitude ofless than 8 nT, or the solar wind electric field of less than about 4 mV/m that the data cover the entire high-latitude region. The purpose of this study is to construct the empirical model that can predict the potentialdistribution for the extreme solar wind condition as well as the average solar wind condition. First, we obtainedthe potential distribution for the average solar wind condition as a function of the IMF and the solar wind electricfield by analyzing the DE-2 data statistically. We then compared those potential distributions with the observationfrom the limited passes of DE-2 for the extreme solar wind condition and with the observation from the similarspacecraft, which can be found in the literature, and examined how the obtained functions for the average solarwind condition can be extended to the extreme solar wind case. We present the result of the potential modelingfocusing on the variation of the pattern during the course of the storm.

- 107 -

P1-026

Possible Effects of Solar and Geomagnetic Activity on AccidentsFamil R. Mustafa1, Svetla Dimitrova2, Elchin S. Babayev1, Irina Stoilova2, Vladimir N. Obridko3, and Katya Georgieva2

1. Shamakhy Astrophysical Observatory (ShAO) named after N.Tusi and Laboratory of Heliobiology, Azerbaijan NationalAcademy of Sciences2. Solar-Terrestrial Influences Laboratory at the Bulgarian Academy of Sciences3. IZMIRAN of Russian Academy of Science, RUSSIA

This study is an attempt to assess the effect of solar activity (SA) and geomagnetic activity (GMA) on any kind ofaccidents registered at Emergency and First Medical Aid Stations of grand Baku area for the period 2003-2005covering 30 588 cases.Analyses of variance (ANOVA) were employed to check the significance of the influence of GMA and the type ofgeomagnetic storms: those caused by magnetic clouds (MC) and by high speed solar wind streams (HSSWS) onthe accidents. The results obtained revealed as other similar investigations that there was a significant decrease of accidents withGMA increase when SA goes to minimum. The accident number started decreasing two days prior to geomagneticstorms, estimated by averaged diurnal value of Dst-index, and was less up to 3 days after them.It was established that accidents increased significantly two days before, one and three days after development ofgeomagnetic storms caused by MC. This result indicates that probably different geomagnetic storms affect on adifferent way on the human physiological and psycho-physiological state.

P1-027

ERG Project : Japanese Geospace ExplorationT. Ono1, Y. Kasaba1, A. Kumamoto1, M. Hirahara2, T. Takashima3, A. Matsuoka3, K. Asamura3, K. Shiokawa4, K. Seki4, and Y. Miyoshi4

1. Graduate School of Science, Tohoku University, Sendai, Japan2. Rikkyo University, Tokyo, Japan3. JAXA/ISAS, Sagamihara, Japan4. STE Lab., Nagoya University, Nagoya, Japan

For the purpose to study the unresolved major problems underlying in Geospace, ERG (Energization andRadiation in Geospace) project has been proposed being focused on the evolution of radiation belts associatedwith magnetic storms. The project consists of three parts; the ERG satellite, the ERG ground network, and theERG modeling/ data center. The ERG satellite is designed to make in-situ observation of the storm time particlesand fields to evaluate the adiabatic and non-adiabatic processes which control the dynamics of relativisticparticles. The instruments on-board are assigned as following; (i) measurement of the distribution functions ofelectrons and ions in wide energy range such as 10eV to 10MeV for electrons and 10eV to 1MeV for ions, (ii)measurement of DC electric and magnetic fields with resolution of 0.1mV/m and 0.1nT, and (iii) measurement ofelectric and magnetic components of plasma waves in a frequency range from 1Hz to 5MHz. The ERG project also involves ground-based observation facilities of optical measurements (6 stations),Super-DARN HF radars (10 stations), 210 deg. meridian magnetometer network (25 stations) and CPMN chain(10 stations) which make it possible to detect of geomagnetic and ionosphere disturbances associated withgeomagnetic storms. The ERG modeling/data center is the facility to examine the comprehensive data setcomparing with the results of computer simulation of particles and fields in the Geospace. The ERG project teamis also planning to collaborate with THEMIS, RBSP (NASA) and ORBITALS (Canada) missions. The ERG proposal was submitted to ISAS/JAXA as a category of small scale satellite mission. The ERG satelliteWG has been established in ISAS/JAXA as the category of pre-phase-A.

- 108 -

P1-028

Development of Auroral Acceleration Regions at Substorm Onsets asDerived from AKR SpectraA. Morioka1, Y. Miyoshi2, F. Tsuchiya1, H. Misawa1, T. Sakanoi1, K. Yumoto3, R. R. Anderson4, J. D. Menietti4, and E. F. Donovan5

1. Planetary Plasma and Atmospheric Research Center, Tohoku University, Sendai, Japan2. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Japan3. Space Environment Research Center, Kyushu University, Fukuoka, Japan4. Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA5. University of Calgary, Canada

The vertical structure and its dynamics of the AKR source region prior to and during a substorm were investigatedusing the Polar/PWI data. Dual AKR sources at substorm onset were identified: a low-altitude one and ahigh-altitude one. The low-altitude source appears in the substorm growth phase at 4000 to 5000 km, and itsintensity increases a few minutes prior to substorm onset. The high-altitude source abruptly appears at substormonset in the altitude range from 6000 to 12,000 km with a remarkably fast growth rate. These AKR features atsubstorms were discussed in relation to the development of the auroral acceleration region. It was suggested thatthe low-altitude AKR source is related to the large-scale inverted-V acceleration region that would be generatedthrough the self-consistent distribution of the magnetospheric plasma in the M-I coupling region. Thehigh-altitude AKR source which is an indicator of a substorm onset would be generated from the localfield-aligned acceleration due to the current-driven instability or the Alfvenic acceleration caused bysubstorm-associated short wavelength Alfven waves.

P1-029

Importance of Equatorial Ionospheric Scintillation in Space WeatherStudiesS. Banola and B.M.Pathan

Indian Institute of Geomagnetism, Plot No.-5,Sector-18, New Panvel (W),Navi Mumbai-410218, INDIA

'Space Weather' gives quantitative description of the physical changes in the near-earth space environment inresponse to variation in solar radiation, solar plasma ejections, and electromagnetic status of the interplanetarymedium. Plasma density irregularities in the ionosphere (associated with ESF, plasma bubbles and Sporadic Elayers) cause scintillations in various frequency ranges. VHF radio wave scintillation technique is extensivelyused to study sub-kilometre scale-size plasma density irregularities. Effects of magnetic and solar activity onionospheric irregularities are studied so as to ascertain their role in the space weather of the near earthenvironment in space. Indian Institute of Geomagnetism operated a ground network of 13 stations monitoringamplitude scintillations on 244/251 MHz (FLEETSAT 73E) signals in India for more than a solar cycle underAICPITS. At present VHF scintillation is being recorded at Mumbai by monitoring 251 MHz signal transmittedby geostationary satellite UFO. Occurrence of daytime scintillations was higher than the nighttime scintillationsduring CAWSES campaign (March-April 2006, low sunspot period). To study solar cycle association ofscintillation, long series of simultaneous amplitude scintillation data for the period Jan. 1989 to Dec. 2000 atIndian region are utilized. Geomagnetic control on the width of the scintillation belt is studied from the latitudinalvariations of scintillation occurrence separately for geomagnetic quiet and disturbed days and also for the groupsof days with low, medium and high Ap values. Nighttime scintillation occurrence is solar activity dependent. It isnoticed that with increase in geomagnetic activity at low and equatorial regions scintillation occurrence isinhibited. The detailed results will be presented.

- 109 -

P1-030

Cosmic Ray Intensity Variation in the Interplanetary Medium Observed byGround-based DetectorsMarlos R. da Silva1, Ezequiel Echer1, Alisson Dal Lago1, Walter D. Gonzalez1, Aline de Lucas1, Luiz Eduardo A. Vieira2, Fernando L. Guarnieri2, Nelson J. Schuch3, Takao Kuwabara4, and Kazuoki Munakata5

1. Instituto Nacional de Pesquisas Espaciais - INPE, Brazil2. Universidade do Vale do Paraiba - UNIVAP, Brazil3. Centro Regional Sul de Pesquisas Espaciais - CRSPE, Brazil4. Bartol Research Institute, USA5. Department of Physics, Shinshu University, Japan

This work shows the dependence of the secondary cosmic rays (muon and neutrons) on the solar wind magneticstructures observed in the interplanetary medium. We have analyzed interplanetary and cosmic ray ground baseddata from 2001 to 2004. Interplanetary magnetic field and solar wind plasma data were taken from the instrumentson board the Advanced Composition Explorer - ACE satellite. Ground based cosmic ray data were take from theneutron monitor maintained by the Bartol Research Institute of the Delaware University, United States, and themuon scintillator telescope, installed in the Southern Space Observatory - SSO in Sao Martinho da Serra, Brazil.With the knowledge of the cosmic ray behavior and its modulation by solar structures, we can sense remotely thisstructures observing the cosmic ray anisotropy in the interplanetary medium. We observed that, during the passageof magnetic clouds, cosmic ray decreases are larger than during the other structures. Furthermore, the cosmic rayresponse to the corotating interaction region passage is the less intense. In spite of all efforts, it is not possible tosatisfactorily explain the cosmic ray response during the passage of the interplanetary structures, but severalmodels and observations attribute the cosmic ray decreases mainly to the particle scattering in the turbulentmagnetic field area between the shock front and the ejecta.

P1-031

A Simple Program to Calculate Satellite's ReentryAbdul Rachman

National Institute of Aeronautics and Space (LAPAN), Bandung 40173, Indonesia

A computer program has been developed to predict the time of satellite's reentry. This simple program alreadytakes account of space weather effects represented by solar and geomagnetic activity. Because of its simplicity,this program can only be used to obtain preliminary results.

- 110 -

P1-032

Double-dip Development of Storm Main Phase Observed in the LowLatitude Geomagnetic RecordsRashmi Rawat, Sobhana Alex, and Gurbax Singh Lakhina

Indian Institute of Geomagnetism, Plot No. 5, Sector-18, New Panvel (W), Navi Mumbai-410218, Maharashtra, INDIA

Complex interaction of the solar wind and the magnetosphere is a topic of extensive research for the past twodecades. Various sporadic solar manifestations like solar flares, coronal mass ejections and coronal holes serve asmajor sources of solar electromagnetic and particle emissions. These transient powerful eruptions drive theinterplanetary (IP) shocks which impinge on the magnetosphere and compress it. Consequently, transfer of solarwind energy into the magnetosphere takes place by magnetic reconnection, wherein the southward oriented Bzcomponent of interplanetary magnetic field (IMF) re-connects with the oppositely directed geomagnetic field. Fora typical geomagnetic storm, subsequent to the interplanetary shock compression producing the storm suddencommencement, the main phase is known to follow the southward traversal of IMF Bz. Dominant main phasecharacteristics in correspondence with the persisting duration of southward interplanetary magnetic field, arecontrolled by the energy influx during the interaction of solar wind and the magnetosphere. In the present study,an attempt is made to depict the salient features of double-dip main phase development conditions as observed inthe geomagnetic field variations in the equatorial and low latitude digital magnetic records from the Indianlongitude for solar cycle-23. Differing energy inputs during such events are discussed by presenting a quantitativeestimate of various magnetospheric current systems during the double-dip storms in comparison with intense mainphase storms.

P1-033

Solar Flare Effect on Subionospheric VLF Transmitter Signals Received atLow Latitude in the South Pacific RegionAbhikesh Kumar and Sushil Kumar

School of Engineering and Physics, The University of the South Pacific, Suva, Fiji

Six VLF transmitter signals with call signs NWC (19.8 kHz, 21.8?&#65533; S, 114.2?&#65533;E), NPM (21.4kHz, 21.4?&#65533;N, 158.2?&#65533;W), IND (18.2 kHz, 8.5?&#65533;N, 77.8?&#65533;E), NLK (24.8 kHz,48.2?&#65533; N, 121.9?&#65533;W), NAA (24 kHz, 44.7?&#65533;N, 67.3?&#65533;W) and NTS (18.6 kHz,38.5?&#65533;S, 146.9?&#65533;E) are monitored at a low latitude station Suva (18.2?&#65533;S,178.5?&#65533;E), Fiji. The Transmitter Receiver Great Circle Paths (TRGCP) range from 3.8 to 11.4 Mm. Theamplitude and phase of above transmitter signals are logged at a resolution of 10 Hz using SoftPAL dataacquisition system. The effect of recent solar flares with classes X6.5 to B8.5 that occurred on 06 November 2006,06-14 December 2006 and 29 January 2007 and caused amplitude and (or) phase perturbations of the VLF signalswill be presented. Solar flare effect was observed only when TRGCP was entirely or partly in the daylight region.All the flare induced perturbation on the VLF signals showed an enhancement in the amplitude but not always inphase. The amplitude enhancements of up to 10 dB from normal level with effect lasting to about 1.5 hours havebeen observed. The GOES X-ray flux data are found to correspond very well in the time and the level ofamplitude and phase enhancements during the strong flares. The enhanced X-ray flux due to solar flares causes asignificant lowering of the VLF reflection height of the D-region of the ionosphere (or increase in electrondensity) that enhances the amplitude and (or) phase of the subionospheric VLF transmission.

- 111 -

P1-034

The Persistence of Equatorial Spread F - An Analysis on Seasonal, SolarActivity and Geomagnetic Activity AspectsV. Sreeja, C.V. Devasia, Sudha Ravindran, and R. Sridharan

Space Physics Laboratory, Vikram Sarabhai Space Center, Trivandrum 695022,India

One of the important aspects of the Equatorial Spread F (ESF) occurrence namely, the persistence of ESF isaddressed to starting from the behavior of the phenomena during different seasons and geomagnetic activity levelsunder the maximum and minimum solar activity conditions at the magnetic equatorial location of Trivandrum(8.5N; 77E; dip lat. 0.5 degree) in India. Based on a detailed analysis of the ionograms recorded at this locationduring the solar maximum year (2001) and minimum year (2006), it is shown that one could estimate the durationof ESF by knowing the magnitude of the F region vertical drift velocity (Vz) associated with the evening time PreReversal Enhancement (PRE) of the F region zonal electric field and the magnetic activity index Ap, for thatparticular day. Any sort of advance information on the possible duration of persistence of the ionosphericirregularities responsible for ESF is important for the understanding the scintillation morphology because of itseffect on space based communication and navigation.

P1-035

Electrodynamic Coupling between High- and Low-latitudes --Characterization and ModelingR. Kombiyil1, C. Mazaudier2, K. Yumoto3, Y. Kasaba1, T. Uozumi3, M. Ito3, and A. Ikeda3

1. Dept. of Geophys., Tohoku University, Aramaki-aoba, Aoba-ku, Sendai, 980-8578, Japan2. CETP/CNRS, 94107 Saint-Maur-des-Fosses Cedex, France3. Space Environment Research Center, Kyushu University 53, 6-10-1 Hakozaki, Fukuoka, 812-8581, Japan

The external component of the Earth's magnetic field is characterized by transient variations. These have temporalscales ranging from a minute to several hours and cause coherent fluctuations in the observed ground magneticfields at high-latitude as well as on the dayside dip equator. Our aim is to study electrodynamic coupling betweenhigh- and low-latitudes during disturbed conditions. The external ground magnetic field arises as a result of thesuperposition of different current systems in the ionosphere and the magnetosphere. They need to be addressedusing case-based arguments, since quantifying them is difficult task. We analyze the DP fields for different eventsassociated with storm, substorm, and the coherent (on a global scale) DP2 variations. To this end, we mainly usedata from the Japanese 210mm meridional chain and make use of other magnetometer (Intermagnet network etc.)chains for comparison. We have calculated ionospheric sheet currents flowing in the E-region (~110km) frommagnetic data and plan to make use of other electrodynamic parameters (observations/computed) for investigatingthe state of the equatorial ionosphere during times of penetration of electric fields and currents induced bymagnetospheric sources.

- 112 -

P1-036

Detection of Seismo-Electromagnetic SignaturesShourabh Bhattacharya, Shivalika Sarkar, and A.K.Gwal

Space Science Laboratory, Department of Physics, Barkatullah University, Bhopal, India

Earthquakes are considered as a major geophysical hazard today. Recent times have impressed the scientificcommunity with results of electromagnetic signatures that have been detected using space borne techniques andtheir continuous study helps in establishing them as short term precursors to seismic events. A major developmentin this regard has been the launch of DEMETER satellite, aimed at detection of ionospheric perturbations linkedwith seismic activities. In this paper, the authors present some interesting examples of electromagnetic signatureswhich have been observed before some earthquakes in the recent times with the help of DEMETER satellite.These seismo-electromagnetic signatures may be regarded as a passive phenomena related to space weather eventsas they play an influential and indirect role to space weather events due to their presence being detectable in theionosphere.

P1-037

Numerical Modeling of the Behavior of the foF2 during Substorm withCurrent WedgeMaxim V. Klimenko1, Vladimir V. Klimenko2, and Valerij V. Bryukhanov1

1. Kaliningrad State Technical University, 1, Sovetsky Av., Kaliningrad, 236000, Russia2. West Department of IZMIRAN, 41, Pobedy Av., Kaliningrad, 236017, Russia

The numerical calculation results of ionospheric effects of modeling substorm which have begun in 18 UT arepresented. Calculations are executed on the basis of Global Self-consistent Model of the Thermosphere,Ionosphere and Protonosphere, developed in WD IZMIRAN, added by the new block of calculation of electricfields in the ionosphere. In calculations we considered superposition of magnetospheric convection electric field(at set of field aligned currents of the first and second zones and substorm current wedge) and dynamo field. It isshown, that at early stage of substorm development the longitudinal extent of main ionospheric trough increases.The trough is stretched in evening sector of southern hemisphere. There is foF2 increase in southern polar cap thatleads to increase in steepness of trough polar edge. Longitudinal extent of equatorial anomaly in evening sectordecreases. In quiet conditions in southern hemisphere the main ionospheric trough is the deepest in post-midnightsector. During substorm the additional minimum in evening sector is formed. In northern polar cap the substormwithout taking into account current wedge leads to little changes foF2. The substorm with taking into account ofcurrent wedge causes negative foF2 disturbances in night and evening sectors of northern polar cap. Depth ofmain ionospheric trough in northern hemisphere decreases. There is strongly reduction of longitudinal extent ofequatorial anomaly in post-sunset sector during substorm without taking into account current wedge. In the furtherthe depth of main ionospheric trough is decreased.

- 113 -

P1-038

Excitation of Quasi-electrostatic Waves in the Ring Current RegionS. V. Singh, A. P. Kakad, R. V. Reddy, and G. S. Lakhina

Indian Institute of Geomagnetism, New Panvel (W), Navi Mumbai-410218, India

During the geomagnetic storm ring current is populated with energetic particles such as hydrogen (H+) andoxygen (O+) ions. These ions have anisotropic distribution functions that can provide free energy for theexcitation of different types of plasma waves in the ring current region. The compositional variations of these ionscan affect the ring current plasma dynamics. Quasi-electrostatic waves with frequencies greater than the protoncyclotron frequency are studied in the ring current region taking into account of pressure anisotropy of H+ and O+ions. The propagation of these waves is considered to be oblique to the ambient magnetic field. The purpose of thestudy is to understand the wave-particle interaction in the ring current region. The low-frequency waves studiedhere are expected to scatter the ring current particles into the loss-cone and hence leading to the ring currentdecay. This mechanism of ring current decay through wave-particle interaction may be complementary to chargeexchange process of ring current decay.

P1-039

The Orbit Characteristic of LAPAN TUBSAT SatelliteNizam Ahmad

National Institute of Aeronautics and Space (LAPAN), Jl.Dr.Djundjunan 133, Bandung 40173, Indonesia

LAPAN TUBSAT is the first video surveillance micro satellite belongs to Indonesia. It was launched on January10, 2007 and has been placed in polar orbit (i= 98 deg) and altitude about 630 km. The orbit characteristic ofLAPAN TUBSAT can be predicted by studying orbit from some micro satellites which identic in the case ofmission and orbit. This study is useful to reduce the failure of its mission. This characteristic included thechanging of orbital elements caused by perturbation forces in space environment which affect satellite mission. InLow Earth Orbit (LEO) the perturbations come from non gravitational force such as atmospheric drag andgravitation force from earth oblatness. From simulation can be predicted that in the early years of its operation, thevariations in altitude and semi major axis are relatively small. It means that this satellite could have the life timemore than 50 years. The effect of earth oblatness will cause the regression of the nodes and the rotation of the lineof apsides, approximately about 1 deg/day and -3 deg/day. These changes are not too critical for polar orbit whichmean that satellite keeps on conducting its mission goal such as satellite imaging.

- 114 -

P1-040

Statistical View of Large-scale Electric Field in the Inner Magnetosphereduring Geomagnetic StormsAtsuki Shinbori1, Yukitoshi Nishimura2, Takayuki Ono2, Atsushi Kumamoto2, and Takashi Kikuchi1

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Furocho, Chikusa-ku, Nagoya, 464-8601, Japan2. Graduate School of Geophysical Institute, Tohoku University, Aramaki Azaaoba, Aoba-ku, Sendai, 980-8578, Japan

In order to clarify temporal and spatial evolutions of large-scale electric field in the inner magnetosphere duringthe geomagnetic storms, we have performed statistical analysis of the long-term electric field observation of theAkebono satellite for about 7 years from March, 1989 to January 1996. In the present data analysis, we definedthe phenomena of magnetic field disturbances indicating the minimum value of less than -40 nT in the SYM-Hindex as the geomagnetic storm. We also identified the magnetically quiet condition when the SYM-H and Kpindices represent more than -20 nT and less than 2. Moreover, we mapped the electric field data into theionosphere using IGRF90 model.In a quiet-time condition, the electric field distribution in the high-latitude region of more than 60 degrees shows atypical structure of the two-cell convection pattern. In the polar cap region, the potential drop was about 26 kV.During the main phase, the electric field intensity increases up to 40-100 mV/m and the polar cap region expandsinto the low-latitude region up to 55 degrees. The polar cap potential drop was about 80 kV. Moreover, a newcomponent of the poleward electric field appears in the sub-auroral latitude region of the dusk sector,corresponding to the SAID/SAPS phenomena.During the recovery phase, the electric field intensity abruptly decreases and the polar cap boundary moves intothe high-latitude region from 70 to 74 degrees. The shielding electric field appears with the magnitude of 5-10mV/m in the middle-latitude region.

P1-041

VESO: Virtual Earth-SunAmerico Gonzalez-Esparza, G. Cifuentes-Nava, J. F. Valdes-Galicia, E. Hernandez-Quintero, and A. Lara-Sánchez

Instituto de Geofisica, Universidad Nacional Autonoma de Mexico, Ciudad Universitaria, Mexico DF 04510A

We present the Virtual Earth-Sun Observatory (VESO) at the web site www.veso.unam.mx. This site shows a realtime integrated data-base obtained from four instruments of the Instituto de Geofisica-UNAM studying Sun-Earthconnection phenomena. (1) The Solar Radio Interferometer (RIS) measures the lower solar atmosphere radiationat 2.5 GHz, revealing bursts associated with solar activity. (2) The Mexican Array Radio Telescope (MEXART)will detect solar wind large-scale disturbances between Sun and Earth (e.g., Interplanetary counterparts of CoronalMass Ejections (ICMES) and Stream Interaction Regions (SIR)) employing the interplanetary scintillationtechnique (IPS) operating at 140 MHz. (3) The Cosmic Ray Observatory detects high energy galactic particles,which flow is affected by large-scale magnetic disturbances in the solar wind. (4) The Teoloyucan GeomagneticObservatory measures the variations in the Earth's magnetic field. The VESO instruments provide data from fourdifferent points of the complex chain of the solar terrestrial relations and will allow the study of intense solarevents causing geomagnetic activity. The VESO project is part of the celebration of the InternationalHeliophysical Year (IHY) in Mexico.

- 115 -

P1-043

Ionospheric Disturbances Detected by GPS Receiver Networks at Mid- andLow-latitudesAkinori Saito1, Michi Nishioka1, Naomi Murakami1, Yuichi Otsuka2, and Takuya Tsugawa2

1. Department of Geophysics, Kyoto University, Kyoto 606-8502, Japan2. Solar-Terrestrial Environment Laboratory, Nagoya University, Toyokawa 442-8507, Japan

The characteristics of Traveling Ionospheric Disturbance (TID), and ionospheric phenomena accompanying TIDwere studied with the GPS-Total Electron Content (TEC) data measured by GEONET, the GPS network operatedby Geographical Survey Institute Japan. The average spacing of GEONET GPS receiver is about 20km. The30-second sampling data of GEONET can observe the ionospheric structures with high spatial and temporalresolution, which is difficult to be obtained by the other observational technique of the ionosphere. In themid-latitude region, the atmospheric gravity waves (AGWs) and tidal waves transport the energy from the loweratmosphere to the upper atmosphere. The physical mechanism of the ionospheric phenomena at mid- andlow-latitudes are complex of the vertical coupling process, latitudinal coupling process, and neutral-ionizedatmospheres coupling process. TID is an example of the phenomena caused by these coupling processes. GPS canbe used as the observational tool of the ionospheric phenomena, and can be affected by the ionosphericphenomena on the other hand. The southern part of Japan is in the geomagnetically equatorial region, and suffersthe interference of the satellite radio waves by plasma bubbles. The ionospheric phenomena, and the ionosphericeffect of the mid- and low-latitude ionospheric disturbances on the GPS-based navigation system, such as MSAS,around Japan will be reviewed in the presentation.

P1-044

Geomagnetic Sudden Commencements (SCs) Observed by Oersted andCHAMP Satellites above the IonosphereT. Araki1, D. Han1, K. Schlegel2, H. Luehr3, and H. Yang1

1. Polar Research Institute of China,China2. Max-Planck Institute for Solar System Research, Germany3. Geoforschungs Zentrum Potsdam, Germany

The geomagnetic sudden commencement (SC) is a good probe to study a transient response of the magnetosphere-ionosphere-conducting earth system to the sudden increase of the solar wind dynamic pressure. Although theprimary source current of SCs is the increased magnetopause current which causes a compression of the wholemagnetosphere, electric currents are induced in various other parts of the system and produce a complex globaldistribution of the amplitude and waveform of SCs. It is important to understand separately a behavior of eachcurrent source. Among them the ionospheric currents are particularly important because they play essential rolesto produce the complex dependence of the amplitude and waveform upon local time and latitude. In order todetect ionospheric currents, a simultaneous magnetic observation above and below the ionosphere is necessary butso far available observations were only from MAGSAT which flew along the dawn-dusk orbit from November1979 to May 1980. Now data are available from observations of Oersted (launched to the orbit of altitude640-850km in February, 1999.) and CHAMP ( 450km, July, 2000). Here we report the results of the initialanalysis of data of both satellites.

- 116 -

P1-045

Equatorial Electrojet (EEJ) Characteristics during Quiet and DisturbedSpace Weather ConditionsB.Veenadhari and S.Alex

Indian Institute of Geomagnetism, Kalamboli, New Panvel, Navi Mumbai-410218, India.

The north-south (Horizontal) configuration of the earth's magnetic field over the equator is responsible for thenarrow band of east-west current system over the equatorial latitudes and is called the Equatorial electrojet (EEJ)and is a primary driver for Equatorial Ionization anomaly (EIA). Equatorial electric fields and plasma drifts playfundamental roles on the morphology of the low latitude ionosphere which undergoes large variability duringgeomagnetically quiet and disturbed periods. An estimation of disturbance index for the equatorial electrojet iscomputed by eliminating the quiet time variation for the disturbed periods as geomagnetic storms. It s well knownthat, during the solar-interplanetary-magnetosphere disturbances, the storm time electric fields, the promptpenetration electric field and delayed disturbance dynamo affects the low latitude ionosphere current system andchanges the F region plasma dynamics. Quantitative study is done to illustrate the development process of EEJand its influence on ionospheric parameters for varying IMF conditions as inferred in the ground geomagneticsignatures using digital geomagnetic and satellite data.During the high solar activity, the dominant role of Coronal Mass Ejections (CMEs) and IMF conditions dominatethe development of the geoeffective magnetic storms. The fast stream high speed solar wind from coronal holeplays major role in development of moderate geomagnetic storms under different IMF conditions, during lowsolar activity periods. During the present solar cycle, campaign observations were made during March - April,2006 under the CAWSES India program. Utilizing the high resolution geomagnetic digital data from low andequatorial latitudes for Indian sector, an estimate the energy injection process during high speed stream coronalhole and associated changes in the solar wind plasma, IMF conditions are examined for various storms occurduring low and ascending phases of present solar cycle.

P1-046

CaII K Spectral Characteristics of Two-Ribbon FlaresHiroko Watanabe1, Reizaburo Kitai2, Tahei Nakamura1, Satoru UeNo2, Takako T. Ishii2, and Kazunari Shibata2

1. Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 607-8471, Japan2. Kwasan and Hida Observatory, Kyoto Unversity, Kamitakara, Gifu 506-1314, Japan

It is well known that some of strong emission lines in the spectra of solar flares show asymmetric profiles. Ichimoto and Kurokawa et al.(1984) reported strong red asymmetry in H alpha line, which implies a downwardvelocity of 40-100km/s in the upper chromosphere. CaII K line profile is also characteristic in solar flares, whichshows red asymmetry at K1(intensity minimum). Fang et al.(1992) indicated that based on Non-LTE calculations,a converging motion around temperature minimum region can well explain the red asymmetry observed at K1position. We present the first results from high-cadence CaII K spectra of two-ribbon flares, observed with Domeless SolarTelescope at Hida Observatory. This flare occured on May 3,2007 in NOAA 10953 and was classified into GOESclass C9.7. The data covers almost the whole period of the flare, from just before the impulsive phase, to aboutthree hours after the peak phase. We also used H alpha multi-wavelength filtergrams to analyze the flaremorphologically.We focused on the CaII K spectral characteristics of flare kernels, that is, strong red shift during the impulsivephase, and tried to search the most suitable atomospheric conditions which produce these properties byMulti-code calculations. This presentation will show you an explanation of observed asymmetry spectra, and ourinterpretations of how the atomospheric conditions change with time and space in flare kernels.

- 117 -

P1-047

Propagation of Coronal Mass Ejections in the Interplanetary MediumMunetoshi Tokumaru, Masayoshi Kojima, and Ken'ichi Fujiki

Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan

We investigated propagation of coronal mass ejections (CMEs) between the sun and the Earth orbit usinginterplanetary scintillation (IPS) measurements of the Solar-Terrestrial Environment Laboratory (STEL) of theNagoya University. In this study, we analyzed data of the scintillation disturbance factor, g-value, derived fromour IPS measurements to determine 3D distribution and motion of CME-associated density enhancements in thesolar wind. As result, we found two types of density enhancements which exhibited different propagation profiles.One of those is a density enhanced region propagating at a comparable speed to the CME-driven shock, and this isascribed to the compressed plasma associated with the shock. The other is a high density region propagating moreslowly than the shock speed, and this region is considered to represent coronal ejecta situated in the rear portion ofa magnetic flux rope. Another interesting finding is that a CME appears to propagate up to 0.5 AU without anysignificant deceleration. This fact may suggest that an acceleration force continues to act on the CME tocompensate a deceleration force by the interaction with the ambient solar wind.

P1-048

Global and Spectral Characteristics of Large-Scale Traveling AtmosphericDisturbances during October and November, 2003Eric K. Sutton, Jeffrey M. Forbes, and R. Steven Nerem

Department of Aerospace Engineering Sciences, University of Colorado, Boulder, CO, USA

During the period spanning late October to early November 2003, several X-class solar flares and coronal massejections occurred causing numerous large-scale traveling atmospheric disturbances (TADs) in the thermosphere.Traditionally, observations of the thermospheric phenomenon have been limited to its manifestation within theionosphere, such as changes in foF2 and hmF2. In this study, however, measurements of neutral density taken bythe CHAMP satellite near 400 km are used to analyze the global and spectral characteristics of large-scaletraveling atmospheric disturbances in the thermosphere. Through further processing and filtering of the rawdensity data, many structures consistent with traveling atmospheric disturbances can be seen. A full spectralanalysis of these structures will be given. The fully self-consistent TIEGCM model will be used to aid with theinterpretation of the results. A movie will be shown illustrating the traveling atmospheric disturbances inherent inthe TIEGCM model.

- 118 -

P1-049

Genesis of a Solar Active Region and the Role of Flares from a TopologicalPoint of ViewSatoshi Morita1, Scott W. McIntosh2, and C. Alex Young3

1. Hida Observatory, Kyoto University, Kurabashira, Kamitakara, Takayama, Gifu 506-1314, Japan2. Southwest Research Institute, 1050 Walnut St., Suite 400, Boulder, CO 80302, USA3. ADNET Systems, Inc. and NASA Goddard Space Flight Center, Mail Code 612.5, Greenbelt, MD 20771, USA

The Sun's trans-equatorial coronal hole is an ideal environment for examining the nature of newly emerged activeregions. A newly emerged prolific flaring active region was studied in detail from its birth to decay, and all 52flares (B5 through X class) were examined using SOHO/EIT 195A, MDI, and TARACE 171A data. This ARinitially had two separated dipoles that merged with each other, changing into a single diffuse dipole. We found atleast 44 of the 52 flares occurred along the same well defined magnetic polarity inversion line (PIL), whichformed between the two dipoles. This PIL appeared to rotate with the proper motion of the negative magneticsource, and started to be less well defined after the rotation angle exceed around 108 degrees. All energetic flaresin this AR occurred after this PIL rotated more than 100 degrees. The correlations between the angle and the AR'sactivities comes from the systematic changes on relative positions between the emerging flux region (EFR) ateach center of the initial dipoles and a pair of the center magnetic sources, which were swapping their locations, inthe quadruple configuration. We found two different processes of topological changes simultaneously existing inthe corona above this AR; (1) between two sets of expanding loops connecting into the initial two dipoles, (2)between the expanding loops above an EFR and sheared loops connecting the central pair magnetic sources. Thepredominant process for flare mechanism was changing with regard to those relative positions at the photosphere.

P1-050

Prompt Response of Nighttime Equatorial Scintillations to GeomagneticDisturbances near the Crest of the Equatorial Anomaly in the IndianLongitude SectorA. DasGupta1, S. Ray1, D. Hui1, and A.Paul2

1. S. K. Mitra Center for Research in Space Environment, University of Calcutta, Kolkata, India2. Institute of Radio Physics and Electronics, University of Calcutta, Kolkata, India

This paper presents a study of the effect of prompt penetration of high latitude electric field to the magneticequator on equatorial irregularity generation and scintillations during geomagnetic storms, based on the time ofsouthward turning of IMFBz, Dst and dDst/dt indices. A geomagnetic storm is said to be intense if minimum Dstis less than -100nT; Bz is less than -10nT for at least 3hours. It is moderate if minimum Dst is less than -50nT; Bzis less than -5nT for at least 2hours. The storm is mild if minimum Dst is less than -30nT;Bz is less than -3nT forat least 1hour. During 1996-2005, there were 33 intense, 52 moderate and 3 mild storms with suddencommencement. Amplitude scintillations of satellite signals at VHF (244MHz) and L-band (1.5GHz) have beenrecorded for more than a decade at Calcutta (22.58deg.N, 88.38deg.E geographic, 32deg.N magnetic dip).Scintillations have been observed for 5 intense and 6 moderate storms respectively during this period. There wasno scintillation at this location near the equatorial anomaly crest in the Indian zone for the remaining 28 intenseand 46 moderate storms. Scintillations occurring within 3 hours of IMF Bz at magnetopause are considered asprompt. The prompt response has been suggested to be due to penetration of high latitude electric field in anundershielding condition. In situ ion density measurements from DMSP satellites have been examined during theabove geomagnetic storms. The DMSP data showed equatorial plasma bubbles corresponding to promptscintillations at Calcutta. On days with no prompt scintillations, equatorial bubbles were generated in a narrowlongitude swath where the southward IMFBz at magnetopause maximized around dusk time.

- 119 -

P1-051

Impact of Climate Change on EgyptElsayed M. Abu El Ella

Geology Department, Faculty of Sciences, Assiut University

There is now little doubt that climatic changes predicted as a result of global warming, present potentiallydramatic and far reaching threats to the environment, human welfare and socio-economic systems on a globalscale. Egypt is potentially one of the countries most at risk from the effects of climate change. It is located in anarid - to semi-arid zone. Global warming is expected to affect Egypt in many ways. In particular, water resources,agricultural resources and coastal zones are expected to be adversely affected. The coastal zone of Egypt extendsfor more than 3,500 km and is the home of more than 40% of the population. Most of these people live in andaround a number of very important and highly populated industrial and commercial cities: Alexandria, Port Said,Damietta, Rosetta and Suez.Low lying land in the Nile delta region is considered to be especially at risk from the effects of any sea level riseresulting from global warming. In particular, the cities of the costal zone of Egypt, which are major industrial andeconomic centers, are expected to experience serious environmental impacts, if no action is taken.The objective of this study is to present a vulnerability assessment of Alexandria city to the effects of sea levelrise, and a general survey of potential impacts of climate change over the area. Remote sensing and GIStechniques are used to assess vulnerability and identify sectors likely to be most seriously impacted. A generalsurvey of the potential effects of climate change on the costal zone of Egypt is also presented.

P1-052

Pre-storm Electron Density Enhancements at Middle LatitudesDalia Buresova and Jan Lastovicka

Institute of Atmospheric Physics of the Academy of Sciences of the Czech Republic, Prague, Czech Republic

Geomagnetic storm-induced ionospheric disturbances have been studied for several decades. Nevertheless, someionospheric features related to geomagnetic disturbances are still not clear and hardly predictable. Substantialincreases of foF2 several hours before the storm onset belong to less explored among them. Here we present astudy of such increases of electron density for 65 strong geomagnetic storms of the current solar cycle, as theywere observed above middle latitudes. 15 out of 65 events were accompanied by significant (>20%) increases offoF2 before the storm onset over European area. We discuss occurrence, latitudinal and longitudinal extent anddependence, as well as height profile of the electron density distribution and possible origin of suchenhancements. All observed pre-storm changes of foF2 exhibited positive deviation from the median mostly in therange of 25% to 40 %. Seasonally, the pre-storm enhancement occurrence peaks in summer and is minimum inwinter. The enhancements tend to occur more often at decay branch of solar cycle. Potential sources/mechanismsof the phenomenon will be briefly discussed.

- 120 -

P1-053

Effects of Recent Space Weather Events on the Interplanetary Medium andGeomagnetic StormsR. M. Jadav1, K. N. Iyer2, H. P. Joshi2, A. K. Jadeja3, Hari Om Vats4, and P. K. Manoharan5

1. Department of Physics, Bahauddin Science College, Junagadh - 362001.2. Department of Physics, Saurashtra University, Rajkot - 360005.3. Christ College, Rajkot.4. A & A Division, Physical Research Laboratory, Ahmedabad.5. Radio Astronomy Centre, NCRA-TIFR, Ooty - 643001.

The paper describes the effects of recent space weather events on the interplanetary medium (IPM) sensed byOoty Radio Telescope. The solar observations by LASCO coronagraph onboard SOHO, GOES X-raymeasurements, satellite measurements of the interplanetary parameters and the geomagnetic storm index Dst areused in the study to understand the space weather effects in the different regions of the solar-terrestrialenvironment. The effects of these events are compared and possible explanations attempted.

P1-054

Coronal Rain as an Indicator of Coronal Heating MechanismsPatrick Antolin and Shibata Kazunari

Kwasan Observatory, Kyoto University, 17 Ohmine cho, Kita Kazan, Yamashina ku, Kyoto shi, Kyoto 607-8471, Japan

Observations of coronal loops in UV lines (with TRACE), in H alpha (with DST at Hida Observatory) and now inthe Ca band with Hinode/SOT often show intensity variations flowing down along coronal loops. Thisphenomenon has been termed Coronal Rain and corresponds to cool condensations (10^4 - 10^5 K) of plasma in ahotter surrounding (~ 10^6 K) that form along coronal loops (De Groof et al. 2004). 'Catastrophic cooling' hasbeen proposed as a possible explanation for coronal rain (Muller et al. 2003, 2004, 2005). This consists on the factthat a coronal loop that is only heated at the footpoints can become thermally unstable and rapidly cool down atthe apex, radiative losses overwhelming conductive flux heating. Observations show plasma condensations thataccelerate when falling, reaching velocities of 100 km/s, and in most cases without decelerating. Also, coronalrain seems to be a recurrent phenomenon of the corona. These properties of coronal rain have been so far veryhard to model numerically. In this work we analyse coronal rain observed in the Ca band with Hinode/SOT. Wethen attempt to simulate the phenomenon using the two most popular candidate mechanisms for coronal heating:Alfven wave heating and nanoflare heating. The first model is a 1.5-D MHD code in which Alfven waves aregenerated at the photosphere in response to footpoint shuffling and dissipate their energy through shocks(following the work of Moriyasu et al. 2004). The second model is a 1-D HD code in which numerous heatingevents with nanoflare-like energies are concentrated randomly at the footpoints. The nanoflare heating simulationsoffer a scenario in which cool condensations appear with properties that seem to match coronal rain observations.On the other hand, the Alfven wave heating scenario fails to reproduce the phenomenon, due to the uniformlydistributed shock heating. Coronal rain is thus found to be intimately linked to the heating mechanism as well asto the localization of the heating. Further, being observationally easy to detect, it constitutes an importantdiagnostic tool that could indicate the operating coronal heating mechanism.

- 121 -

P1-055

3D Reconstructions Using Interplanetary Scintillation (IPS) and the SolarMass Ejection Imager (SMEI) DataMario M. Bisi1, Bernard V. Jackson1, Periasamy K. Manoharan2, Richard A. Fallows3, Masayoshi Kojima4, Munetoshi Tokumaru4, Andrew R. Breen3, P. Paul Hick1, Gareth D. Dorrian3, John M. Clover1, and Andrew Buffington1

1. Centre for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive #0424, La Jolla, CA92093-0424 U.S.A.2. Radio Astronomy Centre, TATA Institute of Fundamental Research, Ughagamandalam (Ooty), Tamilnadu, India3. Institute of Mathematical and Physical Sciences, University of Wales, Aberystwyth, Penglais Campus, Aberystwyth, SY233BZ U.K.4. STELab, Nagoya University, Furo-cho Chikusa-ku, Nagoya, Aichi, 464-8601, Japan.

Combined interplanetary scintillation (IPS) and Solar Mass Ejection Imager (SMEI) remote-sensing observationsprovide a view of the solar wind at all heliographic latitudes and solar elongations; from ~180 degrees anti-solar,down to coronagraph fields-of-view. They can be used to study the evolution of the solar wind, solar transients(such as mass ejections), and corotating structures out into interplanetary space, both in scintillation-level and invelocity for IPS, and in Thomson-Scattered white-light brightness for SMEI. Here, we show comparisons ofevents reconstructed using differing IPS systems and SMEI (such as those in early November 2004 observed bySTELab, ORT, and SMEI) by using a 3D reconstruction technique that obtains perspective views from solarcorotating plasma and outward-flowing solar wind as observed from the Earth by iterative fitting of a kinematicsolar wind model to the different data sets. We also make comparisons of the structures seen in the 3Dreconstructions with in-situ measurements such as those from ACE and Ulysses dependent upon the location(s) ofspacecraft.

P1-056

Power Girds GIC Measurement in Hokkaido, JapanShinichi Watari1, Manabu Kunitake1, Kazuhiro Ohtaka1, Keiko Asai1, Kentarou Kitamura2, Tomoaki Hori3, Takashi Kikuchi3, Kazuo Shiokawa3, Nozomu Nishitani3, Ryuho Kataoka4, Yohsuke Kamide5, Teruo Aso6, Yuji Watanabe6, and Yuji Tsuneta6

1. National Institute of Info. and Com. Tech., 4-2-1 Koganei, Tokyo 184-8795, JAPAN2. Tokuyama College of Technology, 3538 Takajo, Kume, Shunan, Yamaguchi 745-8585, JAPAN3. Solar-Terrestrial Environment Lab. of Nagoya Univ., Furo-cho, Chikusa-ku,Nagoya 464-8601, JAPAN4. RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, JAPAN5. Research Institute for Sustainable Humanosphere of Kyoto Univ., Gokasho, Uji, Kyoto 611-0011, JAPAN6. Hokkaido Power Co. Inc., 2-1 Tsuishikari, Ebetsu, Hokkaido 067-0033, JAPAN

There have been numerous reports showing that the space weather influences power grids by geomagneticallyinduced current (GIC). Generally power grids consist of power lines connected both end of the transformers, ofwhich neutral points are grounded directly. Current flows in those circuits if the ground level potential is causedby geomagnetic variations. These currents can damage power grids such as transformers.The effect of GIC is believed to be small in Japan because Japan is located in geomagnetically low latitudes. Toincrease knowledge of GIC, however, GIC measurements have been conducted in Memanbetsu, Hokkaido sincethe end of 2005 jointly by the National Institute of Info. & Com. Tech. (NICT), Hokkaido Electric Power Co.,Inc., and Solar-Terrestrial Environment Lab. (STEL) of Nagoya University.In this presentation, we will report the initial result of a statistical study of GIC on the basis of the data coveringthe measurements for of the first one and half year period. Several GIC events associated with geomagneticstorms are also reported: for example, the intense GIC event of 14-15 December, 2006. This GIC event wasobserved during the largest geomagnetic storm since the beginning of our GIC measurements. The source of thisgeomagnetic storm was the full halo CME associated with the X3.4/4B flare at 2:14 UT on 13 December. Theinterplanetary disturbance took only 36 hours to travel from the Sun to the Earth.

- 122 -

P1-057

Early Results from the SuperDARN Hokkaido RadarNozomu Nishitani1, Tadahiko Ogawa2, Takashi Kikuchi1, Ryuho Kataoka3, Keisuke Hosokawa4, Yoshizumi Miyoshi1, Natsuo Sato5, Hisao Yamagishi5, Akira Sessai Yukimatu5, and Hokkaido HF Radar Group

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan2. Solar-Terrestrial Environment Laboratory, Nagoya University, Toyokawa 442-8507, Japan3. RIKEN, Saitama 351-0198, Japan4. The University of Electro-Communications, Tokyo 182-8585, Japan5. National Institute of Polar Research, Tokyo 173-8515, Japan

Initial results of the SuperDARN Hokkaido radar (geographic coordinates: 43.53, 143.61) will be presented. It is the second mid-latitude SuperDARN radar, and the first one in the Asian sector. It started operation onNovember 20, 2006 after a radio license was issued, and became fully operational after December 2. So far wehave observed a wide variety of phenomena, such as SAPS/SAID type events, poleward flows near the cusp,dayside/nightside TIDs and so on. In this paper we focus on the poleward flow in the dayside region observed during a large storm on December14-15, 2006. The Dst index was as low as -147 nT when the Hokkaido radar was in the dayside region. The radarobserved intense poleward flows up to 1000 m/s, and the flow region ranged from 62 to 58 degs geomagneticlatitudes. Detailed analysis of the radar data during this storm will be presented.

P1-058

SuperDARN Hokkaido Radar Observations of Subauroral IonosphericConvection during Magnetic StormsRyuho Kataoka1, Nozomu Nishitani2, Yusuke Ebihara3, Keisuke Hosokawa4, Tadahiko Ogawa2, Takashi Kikuchi2, and Yoshizumi Miyoshi2

1. RIKEN (The Institute of Physics and Chemical Research)2. STEL, Nagoya University3. IAR, Nagoya University4. UEC

SuperDARN Hokkaido HF radar at 43.53 N and 143.61 E in geographic coordinates (L~1.5), capable ofmeasuring the subauroral ionospheric plasma convection, has been in continuous operation since the beginning ofDecember 2006. Hokkaido radar successfully observed dayside merging, over-shielding, SAID/SAPS, andsub-auroral flow reversal, shedding new light in the physics of the storm-time ionosphere. We report initial resultsabout the interesting ionospheric backscatters obtained during two typical CIR and CME storms, comparing witha ring current simulation.Particularly, we show first 2D observation of a convection flow reversal in sub-auroral post-midnight sector at 1-3MLT during the CIR storm main phase on 29 January 2007. The shear region is extended over 20 degrees inlongitude and five degrees in latitudes, lasting for about 10 min twice, and the flow speed is about 0.5-1.0 km/s.The spatial/temporal variation of the convection flow reversal is successfully reproduced by the ring currentsimulation, suggesting that the flow reversal is produced by the region 2 field-aligned current associated with thering current enhancement.

- 123 -

P1-059

Ion Heating within an Enhanced Westward Convection Channel in theDusk-side IonosphereSawako Maeda1, Yasunobu Ogawa2, Satonori Nozawa3, Shin-ichiro Oyama3, Keisuke Hosokawa4, and Asgeir Brekke5

1. Faculty for the Study of Contemporary Society, Kyoto Women's University, 35 Kitahiyoshi, Kyoto 606-8501, Japan2. National Institute of Polar Research, 1-9-10 Kaga, Tokyo 173-8515, Japan3. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Nagoya 464-8601, Japan4. Department of Information & Communication Engineering, The University of Electro-Communications, 1-5-1 Chofugaoka,Tokyo 182-8585, Japan5. The Auroral observatory, Institute of Mathematical and Physical Science, University of Tromsø, N-9037, Tromsø, Norway

Observations with the EISCAT UHF radars at Tromsoe and Longyearbyen reveal simultaneous enhancements ofthe ion velocity and temperature in the dusk-side F-region ionosphere around 70 degree geomagnetic latitudeduring 12:30-14:00 UT on 19 August 2006. The beams of the two radars pointed to the north and the south fromTromsoe and Longyearbyen, respectively, which enables us to measure the ion velocity and temperature in a samescattering volume at about 330 and 390 km height. The line-of-sight ion temperatures were elevated by about1000-3000 K for a period of the large westward ion flow from 1000 to about 3000 m/sec. The IMF conditionduring the interval of the ionospheric disturbance was the Bz component negative with increasing magnitude from0 to 13 nT and the By component positive with decreasing magnitude from 17 to 9 nT. The SuperDARN HFradars at Hankasalmi and Pykkvibaer observed an enhanced westward convection channel with the peak flowvelocity of 2000 m/sec. The channel approached the heating region from high latitudes and passed over the regionand then went away toward lower latitudes. It is found that the dusk-side ion heating was observed during thepassage of the convection channel.

P1-060

Kinetic Energy Distribution of Twisting Filament EruptionKenichi Otsuji, Reizaburo Kitai, Satoru UeNo, Takako T. Ishii, Shin'ichi Nagata, Goichi Kimura, Yoshikazu Nakatani, and Kazunari Shibata

Kwasan and Hida Observatories, Graduate School of Science, Kyoto University, Japan

We observed a filament eruption on solar limb by Solar Magnetic Activity Research Telescope (SMART) in Hidaobservatory. The observation was done from 1:20 to 2:00 UT on August 4, 2006 with the wavelengths of H alphacenter, plus-minus 0.5 angstrom and plus-minus 0.8 angstrom. From the observation, we derived lateral velocityfrom transversal motion of the filament and line of sight velocity using Beckers' cloud model (Beckers 1964). Asa result, we found that the filament erupted at 30 km/s for the initial 10 minutes then it accelerate to 100 km/s.After the eruption, we observed the filament material fall down to the solar surface at the speed of 80 km/s. Wealso measured the rotational velocity of untwisting motion of the filament, the maximum value of which is about50 km/s.We attempt to measure the kinetic energy of the filament eruption. Using Beckers' cloud model, we can get opticaldepth distribution. From the optical depth of H-alpha line, we can estimate the column mass and total mass ofhydrogen referring to the previous NLTE calculation of typical prominences. Spatial distribution of rotationalenergy and erupting energy will be discussed.

- 124 -

P1-061

Ionospheric Effects of Space Weather Events during the Declining Phase ofthe Solar Cycle 23 Using TEC Measurements from GPSV. Sreeja , C. V. Devasia, Sudha Ravindran, G. Manju, R. Sridharan, and M.R. Sivaraman

1. Space Physics Laboratory, Vikram Sarabhai Space Center, Trivandrum 695022, India2. Space Application Centre, Ahmedabad, India

An investigation is made on the equatorial and low latitude ionospheric response during the January 2005 period,marked by the appearance of two severe magnetic storms: (1) Jan 06-10 2005 (maximum Ap= 179 and Dst= -96 nT) and (2) Jan 16-23, 2005 (maximum Ap= 207 and Dst=-105nT), using data on Total Electron Content (TEC) obtained from the different GPS stations over the Indiansubcontinent in the 77-degree longitude sector. The observed characteristics in the TEC variations during thesetwo events, which occurred in the declining phase of the solar cycle 23, are unique as revealed by the analysisusing TEC maps on the spatial and temporal changes of TEC at different latitudes/longitudes over India. Thedisturbed ionospheric conditions are characterized by the presence of solar flares of class X, M, C, and Brespectively on different days during this period. The effects of these two storms in the TEC variations are studiedalong with the ionospheric and magnetospheric data and the results are presented.

P1-062

Challenges to Multipoint Faraday Rotation Observations of CMEsElizabeth A. Jensen, Bernard Jackson, Mario Bisi, and Paul Hick

Center for Astrophysics and Space Sciences, UC-San Diego, La Jolla, CA 92093, USA

The tomographic analysis of multiple Faraday rotation observations across the plane of the sky can potentiallyprovide a 3D magnetic field vector field of the heliosphere. Faraday rotation is the rotation of the plane ofpolarization of a polarized electromagnetic wave as it traverses a magnetized medium such as the solar corona; itis the integrated product of the electron density and the component of the magnetic field along the line of sight. The Mileura Widefield Array (MWA) can potentially obtain Faraday rotation observations from hundreds ofsources simultaneously and may have the capability to improve our ability to predict the geoeffectiveness ofcoronal mass ejections (CMEs). We will present our results of the effects that a simple Taylor state magnetic fluxrope CME model will have on MWA observations. Our focus is the effect a limited number of sources distributedabout the plane of the sky will have on the analysis of multipoint Faraday rotation observations and the idealdistribution of bandwidth within the capability of MWA for CME observations.

- 125 -

P1-063

Response of Ionospheric Convection to Substorm Expansion Onsets andFast Earthward Flows in the Magnetotail: Geotail and SuperDARNObservationsY. Miyashita1, K. Hosokawa2, T. Hori3, Y. Kamide4, M. Fujimoto1, I. Shinohara1, S. Machida5, T. Mukai1, Y. Saito1, A. S. Yukimatu6, and N. Sato6

1. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 229-8510,Japan2. Department of Information and Communication Engineering, The University of Electro-Communications, Chofu, Tokyo182-8585, Japan3. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8601, Japan4. Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Kyoto 611-0011, Japan5. Department of Geophysics, Kyoto University, Kyoto 606-8502, Japan6. National Institute of Polar Research, Itabashi, Tokyo 173-8515, Japan

Using Geotail and SuperDARN data, we have studied the response of ionospheric convection to two weaksubstorms on 1 May 2001 and its relationship to fast earthward flows in the magnetotail. The Geotail spacecraftwas located in the postmidnight plasma sheet at X ~ -14 Re. While it did not observe fast earthward flows duringthe first substorm, it observed successive fast earthward flows just after the second substorm onset, accompaniedby a clear dipolarization. SuperDARN observations show that the Geotail footprint was located in the equatorwardpart of the dawn cell of the two-cell ionospheric convection pattern. Ionospheric convection in the entire dawn cellstarted to enhance a few min before the expansion onsets of both substorms, regardless of the presence of fastflows at the Geotail location. These results suggest that convection enhancement occurs not only near the footprintof fast earthward flows in the magnetotail but also in the entire ionosphere in association with substorm expansiononset. This is consistent with the previous results of the enhancement of convection in the entire magnetotail.

P1-064

Forcing of the Earth's Atmosphere by Solar StormsKlemens Hocke and Niklaus Kaempfer

Institute of Applied Physics, University of Bern, Sidlerstr. 5, 3012 Bern, Switzerland

The Earth's atmosphere is influenced by solar activitiy as manifestated by sun spots, faculae, and solar flares. Strong solar flares are often associated with interplanetary coronal mass ejections (ICME) which travel at highspeeds through the heliosphere and cause severe disturbances of the Earth's magnetosphere, ionosphere, andupper atmosphere. We select the strongest flares of the solar cycle-23 and perform a superposed epoch analysis using the time series of solar X-ray flux, solar wind speed, planetary geomagnetic activity Ap, and geopotentialheight of the lower troposphere. The typical sequence of the processes is: 1) sun spot darkening in TSI, 2) X-rayburst and faculae brightening in EUV/UV, 3) ICME arrival at the Earth and enhanced geomagnetic activity. Thelower troposphere is not the last link in the Sun-Earth Connection chain, since sun spot darkening disturbs thelower troposphere around 5 days before the solar flare onset.

- 126 -

P1-065

Diurnal Cycles in Middle Atmospheric Water Vapor and Ozone:Measurements and ModelsAlexander Haefele1, Klemens Hocke1, Niklaus Kampfer1, Philippe Keckhut2, and Beatrice Morel3

1. Institute of Applied Physics, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland2. Service d'Aeronomie, Institut Pierre Simon Laplace - CNRS, B.P. 3, 91371 Verrieres-Le-Buisson, France3. Laboratoire de Physique de l'Atmosphere, Universite de La Reunion, B.P. 7151, 97715 Saint-Denis Messag. Cedex 9, LaReunion, France

The datasets of two ground based microwave radiometers measuring water vapor at 22 GHz and ozone at 142GHz located at midlatitudes have been analyzed with respect to diurnal cycles. Both species show diurnalvariations in the order of a few per cent in the stratosphere and mesosphere. At 40 km ozone shows a clearmaximum during late afternoon where water vapor reaches a minimum revealing a clear anticorrelation. The datahas been extensively compared to the MSDOL atmospheric model and to the global scale wave model (GSWM).A very good agreement can be found during summer solstice conditions both for water vapor and ozone. Forequinox conditions the agreement is not distinct in case of water vapor.The diurnal cycles in water vapor at 65 km have been decomposed into a diurnal and a semidiurnal component foreach month. The diurnal component shows a maximum in early summer while the semidiurnal component islargest during winter. This is quantitatively and qualitatively in good agreement with the GSWM. While theamplitudes are underestimated in GSWM compared to the observations in the stratosphere, the phase-altitudedependence is in very good agreement throughout the middle atmosphere.The high time resolution, the fact that the observed volume is fixed in space in contrast to satellite observationsand the big amount of measurement time makes ground based radiometers a good tool to study diurnal variationsand tides.

P1-066

Magnetospheric Response to the Passage of the Solar Wind DiscontinuityEvent on October 21, 1999: A Numerical StudyKhan-Hyuk Kim1, Suk-Kyung Sung1, Kyung Sun Park2, and Tatsuki Ogino3

1. Korea Astronomy & Space Science Institute, Daejeon, 305-348, Korea2. Chungnam National University, Daejeon, 305-764, Korea3. Solar-Terrestrial Environment Laboratory, Nagoya University, Japan

Recently, Shinbori et al. [2004] examined the electric field variations associated with geomagnetic suddencommencements (SC) by using data from the Akebono satellite in the inner magnetosphere (L < 5) and reportedthe following characteristics of the SC-associated electric field variations. (1) The electric field shows a bipolarchange. (2) The initial excursion of the electric field tends to be directed westward. (3) The initial excursion of theelectric field is larger on the dawn/dusk side than near local noon. By using a global three-dimensional MHDsimulation model, we examine how and where such SC-associated electric field variations establish. In our study,we used the SC event occurred on October 21, 1999, caused by a sudden increase in the solar wind dynamicpressure from ~3 to ~13 nPa. The solar wind and interplanetary magnetic field conditions observed from theWIND satellite near GSE (x, y, z) ~ (21.9, -65.4, 2.0) Re are used as the simulation input parameters. Thenumerical simulation shows that inward flow is first excited near local noon and then flow vortices are generatednear the flankside as the solar wind discontinuity is passing over the magnetosphere. Thus, the convection electricfield variations change with local time. The electric fields associated with flow vortices show a bipolar structure.We discuss whether the SC-associated electric fields observed at Akebono are explained by the convectionelectric field obtained from our numerical model.

- 127 -

P1-067

Estimation of the Polar Ionospheric Conductance Using Data from theEISCAT Radar and the Multi-wavelengths PhotometerShin-ichiro Oyama, Taiki Watanabe, Ryoichi Fujii, and Satonori Nozawa

STEL, Nagoya University, Japan

One of the important ionospheric parameters at auroral latitudes is the conductance to study themagnetosphere-ionosphere coupled system. Numerous publications proposed estimating methodology by usingdata taken with the incoherent-scatter (IS) radar and multi-wavelength optical instruments. An advantage of the ISradar in this field is measurement of the height-resolved electron density with good time resolution. While the ISradar provides precise values of the ionospheric conductance, the horizontal coverage may be insufficient toinvestigate horizontally structured ionosphere due to auroral particle precipitation. This disadvantage can besupplemented by using optical data. However, estimating methodology with the optical data has been a concernbecause the emission intensity is related to the conductance in a complicated manner. The best way to establishthe relationship is to compare both data taken in a same volume at the same time. In this case the conductanceestimated from optical data can be calibrated by using that from the IS radar. Then our scientific objective is todevelop the methodology by using simultaneous data from the EISCAT (European Incoherent Scatter) UHF radarand the multi-wavelength photometer. Both instruments are collocated at Tromsoe, Norway (69.6 N, 19.2 E), thusthey can measure the ionosphere along same magnetic field line. The photometer has been operated since October2002. The long-time data set allows us to do statistical studies. In this paper we present statistical relationshipsbetween the conductance from the radar and the emission intensity at several wavelengths.

P1-068

Signatures of Equatorial MTM as Observed from In-situ and Ground BasedIonospheric Measurements in the Indian SectorK. Niranjan1, P.S. Brahmanandam2, and B. Srivani1

1. Department of Physics, Andhra University, Visakhapatnam 530 003, India2. National Central University, Chung-Li, Taiwan

Results of a preliminary study carried out on the features of Midnight Temperature Maximum (MTM) over theIndian sector as observed from the first in-situ electron temperature variations of Indian SROSS C2 RPA data, thethermospheric night airglow intensities at 630 nm recorded from a sub-tropical Indian station Waltair (17.7 N,83.3 E) and a co-located Digital Ionosonde data are reported. The electron temperatures indicate that during thesummer solstice months of low solar activity periods, there was a significant temperature gradient from theequator towards the latitudes of Waltair (14-18 N) from 2200 to 2400 hrs IST even in the topside F-region. Incontrast, during the winter solstice months, temperature contours do not show significant gradient aroundmidnight, though isolated peaks are seen between 0100 to 0300 hrs IST i.e., delayed in time by a couple of hourssuggesting that the MTM is weaker. The MTM induced F-layer descent at sub tropical latitudes due to a probableneutral wind modification and consequent increase in 630 nm night airglow zenith intensity are studied tocharacterize the MTM induced ionospheric changes in terms of the starting time, velocity of F-layer descentindicative of the strength of MTM and the time at minimum height indicative of the time of cessation of MTMinduced perturbation. The results are discussed in the light of earlier work and the current understanding of theorigin of equatorial MTM.

- 128 -

P1-069

Generation Mechanism of Nonthermal Particles in the Distant Magnetotail:Observational Study by GeotailMariko Hirai and Masahiro Hoshino

University of Tokyo, Japan

In the Earth's magnetotail, it is known that nonthermal particles which do not fit into the Maxwell distributionfunction are often observed. Some candidates like magnetic reconnection or turbulent acceleration have beensuggested for the generation mechanism of these nonthermal particles. However, it still remains unsolved whichmechanism plays an important role in the magnetotail where magnetic reconnection often takes place and at thesame time, magnetic turbulence is quite strong. We fitted the three-dimensional velocity distribution function observed by Geotail satellite to the kappadistribution: the distribution based on Maxwell distribution function with long tail which is expressed by powerlow in the high energy regime. We calculated the density, velocity, temperature and power low index by using thefitting method. By statistical study of the plasma sheet, we have shown that the power low index is harder in the distantmagnetotail than that of the near Earth's region. This suggests that the energy density of nonthermal particles isquite dominant (up to 40% of the total energy density) in the distant tail. We will also report on the result of theevent study for both earthward/tailward flow events and discuss the generation mechanism of nonthermal particlesin the distant magnetotail.

P1-070

Nonlinear System Identification Approach to Space WeatherM. A. Balikhin, S. A. Billings, Y. Hobara, and D. Coca

Dept. of Automatic Control & Systems Eng., University of Sheffield, Mappin Street, Sheffield S1 3JD, UK

An overview of nonlinear dynamical systems modelling methodology and its application to space weatherforecasting are presented. Non-parametric methods are used to identify Single Input-Single-Output andMulti-input-single output models for evolution of geomagnetic indices. These models are transferred to thefrequency domain by calculating Generalised Frequency Response Functions (GFRFs). GFRFs are used todeduce continuous time differential equation to describe evolution of geomagnetic indices from discrete models.In the case of the Dst index the identified nonlinear equation is compared with empirical models derived from theBurton model.

- 129 -

P1-071

Space Weather, and Solar and Heliospheric Science with the MileuraWidefield ArrayDivya Oberoi1, Joseph E. Salah1, Colin J. Lonsdale1, Roger J. Cappallo1, and Justin C. Kasper2

1. MIT Haystack Observatory, Route 40, Westford, MA 018862. MIT Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02139

The Mileura Widefield Array is a next generation 80-300 MHz interferometric array expected to come online inlate 2008 in a radio quiet area in Western Australia. Solar and heliospheric science, and space weatherapplications are among the prime science objectives of the array. The array will help bridge the observing gap between observations of the solar surface and satellite measurementsat 1 AU. The large field-of-view and the high sensitivity full polarisation imaging capability of the array will beused to monitor the changes in the Faraday rotation observed towards a large number of astronomical polarizedsources as a Coronal Mass Ejection (CME) crosses the line of sight in order to measure the magnetic field contentof the CMEs. Interplanetary Scintillation observations with the 16 simultaneous sensitive beams will multiply theheliospheric sampling achieved by the array many fold. The high quality point spread function of the array and itscapability to provide high time and spectral resolution data will be exploited to image and study the evolution ofType II and solar bursts. This paper will introduce the instrument and highlight it space weather relatedcapabilities along with the current status of the project.The partner institutions that are developing the array include the MIT Haystack Observatory, MIT Kavli Instituteand Harvard Smithsonian Center for Astrophysics in the US, an Australian consortium involving MelbourneUniversity, Australian National University, Curtin University of Technology, and the Australia TelescopeNational Facility, and the Raman Research Institute in India.

P1-072

Turbulence in Coronal Current Sheets and Successive Particle Accelerationin an Impulsive Solar Flare on 10 Nov 2004Naoto Nishizuka1, Hiroyuki Takasaki1, Ayumi Asai2, Hiroki Kurokawa1, and Kazunari Shibata1

1. Kwasan and Hida Observatories, Graduate School of Science, Kyoto University, Kyoto, Japan2. National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan

Solar flare generates impulsive bursts in some wavelength. Some of them synchronize the brightening of hardX-ray sources, called flare kernels, which are thought to be direct evidence of the particle precipitation into thechromosphere accompanying with the energy release via magnetic reconnection above the coronal magnetic loop. Here we report observations of GOES X2.5class impulsive flare occurred on 10 Nov 2004 made with TRACE,RHESSI and Sartorius Halpha telescope at Kwasan observatory, which show ultraviolet (C IV1550A line) finestructures (~1") and elementary bursts (~2s) in the hard X-ray sources along Halpha two-ribbon flare with hightemporal and spatial resolution. We identify power-law distributions of peak intensity, peak duration and time interval of each peak, whichpower-law indexes are 1.5, 2.2 and 2.5 respectively. This result is similar to turbulence spectrum calledKolmogorov spectrum, indicating the fractal structure in coronal current sheets. Such a turbulent current sheetaccelerate particles intermittently and more rapidly, suggesting the basic physics of the unsteady reconnectionprocess and the particle acceleration process may be common to the impulsive flare burst phenomena.

- 130 -

P1-073

Statistical Study of Multiple Ion Band Structures Observed by the FASTSatelliteYao Yao1, Kanako Seki1, Yoshizumi Miyoshi1, James P. McFadden2, Eric J. Lund3, and Charles W. Carlson2

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8601, Japan2. Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA3. Space Science Center, University of New Hampshire, Durham, NH 03824, USA

During large magnetic storms, so-called multiple ion band structure that is seen as multiple components withdiscrete energies at energy-time spectra was observed in the FAST observations [Seki et al., 2005]. From the casestudy of the April 2001 magnetic storm, Seki et al. [2005] showed that the multiple ion band structure of O+resulted from direct supply from the ionosphere to the inner magnetosphere, and they suggested that the multipleion band structure plays an important role in supplying the O+ ions to the storm-time ring current.In this study, we investigated detailed characteristic of the multiple ion band structure of low-energy O+ ionsbased on the statistical analysis of the FAST data. The data were obtained in the year 2000 that was the solarmaximum period. As a result, O+ bands are mostly observed at CPS and subauroral latitude. On the other hand,H+ bands are in more higher region from 70 to 80 degrees. H+ bands are often observed in quiet time, while O+bands are mostly observed in storm time, especially in intense storm. Moreover, O+ bands are observed in morelower latitude during intense storm time. Magnetic local time dependence of the multiple ion band structure isalso found. O+ bands are mostly observed in dusk side, while H+ bands are observed in night and dawn side.

P1-074

MF Auroral Radio Emissions Observed in IcelandYuka Sato1, Takayuki Ono1, Masahide Iizima1, Atsushi Kumamoto1, Natsuo Sato2, Akira Kadokura2, and Hiroshi Miyaoka2

1. Graduate School of Science, Tohoku University, Sendai, Miyagi, 980-8578, Japan2. National Institute of Polar Research, Kaga, Itabashi, Tokyo, 173-8515, Japan

In order to study the generation and propagation processes of MF auroral radio emissions (referred to as auroralroar and MF burst) in the polar ionosphere, an Auroral Radio Spectrograph (ARS) system was installed atHusafell station in Iceland (invariant latitude: 65.3deg). In late 2006, the ARS detected one auroral roar and twoMF bursts, which were identified as left-handed polarized waves. Results of data analysis including other auroraldata and particle spectra observed by the DMSP satellite suggest that the MF bursts are generated by electronswith an average energy of several keV associated with auroral breakup. On the other hand, the auroral roar isgenerated as upper hybrid waves by relatively low energy electrons over the observation site and propagatesdownward, being converted into L-O mode electromagnetic waves.

- 131 -

P1-075

Spatial Distribution of Non-thermal Microwave Emission in a Solar FlareTakashi Minoshima and Takaaki Yokoyama

School of Science, University of Tokyo, 7-3-1, Bunkyo, Hongo, 113-0033, Japan

High-energy electron trap in a converging magnetic field is a common phenomenon in the Sun and the Earthmagnetosphere. In the Sun, electron trap and its precipitation into footpoints of the magnetic loop are shown byrespective the non-thermal microwave and hard X-ray observations during the flare. Understanding of theirphysics is important for the study of Sun-Earth climate.We describe time evolution of the microwave emission based on the Fokker-Planck treatment of the electron"Trap-plus-Precipitation" model (Melrose & Brown 1976). We especially adress dependence of its spatialdistribution along the loop on; (1) pitch-angle distribution of the parent electrons injected into the loop, and (2)loop geometry and an angle between the line of sight and magnetic field line at the site. Comparing thesecalculation results with the observations, we discuss physical properties of the trapped and injected electrons.Yokoyama et al. (2002) reported microwave propagating feature during the flare. They interpreted it as motion ofa relativistic electron with a pitch-angle of ~70 degree. We reconsider their observation based on our modelcalculation. Our calculations give different interpretation on their observation; microwave propagating featuremay be as a consequence of motion of an ensemble of electrons, which have different frequency of the bouncemotion in the loop due to their initial pitch-angle and thus have different period to emit strong microwave.

P1-076

SC-associated Ionospheric Electric Fields at Low Latitude: FM-CW RadarObservationAkihiro Ikeda1, Kiyohumi Yumoto2, Manabu Shinohara2, Kenro Nozaki3, Akimasa Yoshikawa1, and Atsuki Shinbori4

1. Department of Earth and Planetary Sciences, Kyushu University, Fukuoka,Japan2. Space Environment Research Center, Kyushu University, Fukuoka, Japan3. National Institute of Information and Communications Technology, Koganei, Tokyo, Japan4. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Japan

When SC (geomagnetic sudden commencement) occurs, the intensity of the geomagnetic field increases rapidlyin low-latitude region. Such a step-function like increase of the H-component is called main impulse (MI). Duringthe MI phase, the dawn-to-dusk electric field is penetrated into the polar ionosphere (e.g., Araki, 1994) andtransmits instantaneously into the low-latitude ionosphere (e.g., Kikuchi et al., 1978). However, the characteristicsof the ionospheric electric fields at the time of MI is not yet clarified sufficiently (Hereafter, we call this electricfield the MI-electric field). In order to measure the ionospheric electric fields, we have installed an FM-CW radar at a low-latitude stationSasaguri, Fukuoka, Japan (M.Lat. 23.2 degree, M.Lon. 199.6 degree). By using the Doppler mode of the FM-CWradar, we can measure vertical drift velocity and virtual height of ionosphere with 10 seconds time resolution. We analyzed 40 SC events within a period from 2002 to 2005. As a result, we found that the MI-electric fielddirects eastward in daytime whose peak amplitude is about 0.50 mV/m around 13:30 LT. While, the MI-electricfield directs westward in nighttime and the peak amplitude is 0.86 mV/m around 01:30 LT. The enhancement in the nighttime sector cannot be explained just by the polar electric field. Hence we concludedthat this is caused by the superimposed effect of the polar electric field and the inductive westward electric fieldassociated with the compressional hydromagnetic wave.

- 132 -

P1-077

Electron Acceleration through Microinstability in Collisionless ShocksTakanobu Amano and Masahiro Hoshino

Earth and Planetary Science, University of Tokyo, Japan

Particle acceleration is one of the most important issues in space plasma physics. The importance of particleacceleration in the context of space weather is also widely recognized. Particle acceleration in large solar flaresand associated Coronal Mass Ejections (CMEs) and interplanetary shocks are thought to be an important subjectof space weather.We focus on particle acceleration in collisionless shocks. Although diffusive shock acceleration is the mostprobable acceleration process, there remains several important problems. Among them, the so-called injectionproblem is probably the most important issue for the particle acceleration efficiency. The injection probablyresults from efficient particle heating and acceleration through microinstabilities in the shock transition region.Therefore, it is important to understand nonlinear evolution of plasma microinstability and associated particleheating and acceleration.We investigate electron heating and acceleration via the Buneman instability excited by the reflected ions using atwo-dimensional electromagnetic particle-in-cell code. Initially, waves propagating nearly perpendicular to thebeam are excited as well as the parallel propagating modes, as predicted by the linear theory. However, nonlineardevelopment shows that only waves whose perpendicular wave number are comparable to the most unstable modeof the Buneman instability survives. This results in the formation of spatially isolated potential structures. Electronheating and acceleration efficiency through the interaction with the potential structures are discussed.

P1-078

Solar Activity Dependence of Ion Upflow in the Polar IonosphereYasunobu Ogawa1, Stephan C. Buchert2, Akihiro Sakurai3, Satonori Nozawa3, and Ryoichi Fujii3

1. National Institute of Polar Research, 1-9-10 Kaga, Itabashi-ku, Tokyo, Japan2. Swedish Institute of Space Physics, Box 537, SE-751 21 Uppsala, Sweden3. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Japan

The influence of solar activity upon ion upflow in the polar ionosphere was investigated using data obtained bythe Tromsoe EISCAT UHF radar over a 20-year period from 1984 to 2004. In agreement with other work we findthat the upward ion upflux is generally high during high solar activity than during low solar activity, but ionupflow events behave the opposite, they are more frequently seen during low solar activity. The altitude whereions start to flow upward also depends on solar activity. The ion upflows occurring at relatively high altitudesbetween 350 and 500 km are accompanied by stronger electric fields and higher electron temperatures during highsolar activity than the more frequent ones during low solar activity. These results suggest that the neutral densityin the thermosphere, which increases with solar activity, controls the ion upflow via ion-neutral collisions.

- 133 -

P1-079

Higher-Order Statistics of MHD Turbulence Data Using Multi-SpacecraftMeasurementTohru Hada1, Yasuhiro Nariyuki1, and Yasuhito Narita2

1. ESST, Kyushu University, Kasuga 816-8580, Japan2. IGEP, TU Braunschweig, D-38106 Braunschweig, Germany

Large amplitude magnetohydrodynamic (MHD) waves are ubiquitous in the solar wind. They are believed to playessential roles in various physical processes such as coronal heating and transport of energetic particles. FromMHD turbulence point of view, due to the large amplitude of the waves, one has a possibility to directly observenonlinear interaction among the waves. It is thus important and timely to develop robust and accurate methods toextract as much information on the MHD waves as possible using the field and plasma data obtained bymulti-point measurements. After introducing some basic concepts on higher order statistics, we will present ourrecent progress in evaluating higher order coherence among the waves both in time and spatial domains usingspacecraft data. Some examples will be given.

P1-080

Geomagnetic Activity Induced Tropopause Temperature and Wind overEquatorial LatitudeManohar Lal

EGRL, Indian Institute of Geomagnetism, Krishnapuram, Maharajanagar, Tirunelveli, 627011, India

We have studied the influence of severe geomagnetic storm on the Indian equatorial tropopause temperature, and wind variation. The severe and strong (Dst < -100 nT) geomagnetic storm between 2000 and 2005 has beenstudied in the present work. Some of the storms occurred on 7 April 2000, 31 March 2001, 30 Oct 2003, 21 Nov2003, 8 Nov 2004 etc. The change in the tropopause temperature and wind velocity over Indian continentfollowed by the geomagnetic storm is found to be influenced by the solar activity and QBO phase. The effect ofmagnetic storm is prominant on temperature during high solar activity and on wind during low solar activityperiod. The tropopause (200 mb) temperature increases by about 2.5 K during w-phase of QBO and decreases byabout -3 K during E-phase of QBO. The three to five days time lag has been observed between onset of the eventand change in temperature. The time delay between onset of the event and maximum change in temperaturebecomes minimum during transition phase of QBO. The decrease in horizontal wind velocity before onset of theevent during E-phase of QBO has been observed. The pronounced effect has been observed over east coast ofIndia. The effect of magnetic storm on the tropopause temperature and wind velocity is not seen during monsoonperiod. Similar to the horizontal wind velocity, vertical wind velocity also shows the changes in wind velocityfollowed by the onset of the magnetic storm. The zonal wind velocity on 4th April was minimum and it shows notime lag between onset of the event and maximum increase in wind velocity. The wind velocity followed by thegeomagnetic activity found to be distorted in the presence of strong planetary wave at tropopause height.

- 134 -

P1-081

Competing Process between Mirror Instability and L-mode ElectromagneticIon Cyclotron Instability in the MagnetosheathMasafumi Shoji1, Yoshiharu Omura1, Bruce T. Tsurutani2, and Olga Verkhoglyadova3

1. Research Institute for Sustainable Humanosphere, Kyoto University, Gokasho, Uji Kyoto 611-0011, JAPAN2. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive MS 111-113 Pasadena, CA91109-8099, USA3. Institute of Geophysics and Planetary Physics, University of California Riverside, CA 92521, USA

Mirror instability dominates over L-mode electromagnetic ion cyclotron (EMIC) instability in the magnetosheath,although the linear growth rate of the L-mode EMIC wave is higher than the growth rate of the mirror mode wave. To analyze the competing process between the L-mode EMIC instability and the mirror instability, we comparedthe amplitudes of these modes in two-dimensional and three- dimensional hybrid code simulations. In thethree-dimensional simulation we found that the mirror mode wave can consume more energy than the L-modeEMIC wave at the early stage. In contrast, in two-dimensional simulation, the energy of the L-mode EMIC waveis higher at this stage because its growth rate is larger than that of the mirror mode. This is because the degree offreedom in the oblique angles is increased in three-dimensional simulation. Mirror mode waves which are excitedin the oblique angles to the ambient magnetic field can exist in various regions. We also performed the parametricanalysis of the nonlinear evolutions on the temperature anisotropy of protons. It was also found that the nonlinearevolution of the mirror instability in three-dimensional space is different from that in two-dimensional space.

P1-082

Dependence of the Electromagnetic and Precipitating Particle Energy Inputsto the Ionosphere upon the Sunlit/Shade Condition of the IonosphereRyoichi Fujii1, Hiroshi Handa1, Satonori Nozawa1, and Yasunobu Ogawa2

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan2. National Institute of Polar Research, Itabashi-ku, 173-8515, Japan

Based on an analysis of EISCAT CP-1 data obtained from January 1987 to November 2004, we have statisticallydetermined the dependence of the electromagnetic energy and the kinetic energy of precipitating particles from themagnetosphere into the ionosphere and then thermosphere upon the sunlit/shade condition of the ionosphere. Theenergy deposition by precipitating particles can be derived from the ion-electron pair production rate that isobtained from the recombination rate using measured electron density in the E-region. Since the neutralatmosphere is ionized not only by particle precipitation but also by solar irradiation, however, in order to obtainthe electron density due to particle precipitation, we have first estimated the electron density due to the solarirradiation and expressed it as a function of solar zenith angle by using data where we do not see any significantionizations by particle precipitation. We have thus successfully estimated the precipitating particle energydeposition even in the sunlit ionosphere on all available CP-1 data. The present study shows that not only theelectromagnetic energy but also the precipitating particle energy deposition in the dark ionosphere tends to belarger in the sunlit ionosphere, indicating that ionospheric conditions actively control themagnetosphere-ionosphere (M-I) coupling.

- 135 -

P1-083

Multi-dimensional Superposed-Epoch Analysis of Earth's Magnetotail withGeotail Data and Implied Model of SubstormS. Machida1, Y. Miyashita2, A. Ieda3, D. Nagata1, K. Liou4, T. Nagai5, T. Obara6, Y. Saito2, H. Hayakawa2, and T. Mukai2

1. Department of Geophysics, Kyoto Univ., Japan2. JAXA / Institute of Space and Astronautical Science, Japan3. Solar-Terrestrial Environment Laboratory, Nagoya Univ., Japan4. The Johns Hopkins University, Applied Physics Laboratory, USA5. Dept. of Earth and Planetary Phys., Tokyo Inst. of Tech., Japan6. Applied Electromagnetic Research Center, NICT, Japan

Time development of near-Earth magnetotail during substorms has been investigated by multi-dimensionalsuperposed-epoch analysis with Geotail data. The start time of each substorm was determined by auroral dataobtained by Polar and Image spacecraft. Key parameters derived from plasma and magnetic field data of Geotailwere sorted in the meridional X(GSM) - Z(estimated) coordinates.We could confirm various variations which relevant models of substorm are based on or predict. However, noneof them can perfectly explain our results. Thereby, we propose a new model, in which an earthward convectiveflow starts first about 4 min before the onset, which is caused by the increase of the Poynting flux toward theplasma sheet center resulting in the enhancement of the JxB force. This flow can enhance the occurrencepossibility of the ballooning instability or other instability associated with the current disruption, or the currentdisruption induces the fast earthward flow by the reduction of the pressure gradient force at the earthward edge ofthe stretched current sheet in turn. The formation of the magnetic neutral line is a natural consequence of thepresent model, namely, the relaxation of a highly stretched sling-shot current sheet produces the enhancedduskward electric field first followed by dawn-dusk fluctuations at its tailward edge, which is the boundarybetween the sling-shot current with large stress and the Harris-type current sheet with less stress. Further, inducedflows toward the current sheet center around the boundary may enhance the formation of the magnetic neutralline.

- 136 -

P1-084

What Makes the Difference of Duration between LDE Flares and ImpulsiveFlares?Keisuke Nishida1, Masaki Shimizu1, Daikou Shiota2, and Kazunari Shibata1

1. Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto, 607-8471, Japan2. National Astronomical Observatory of Japan, Mitaka, Tokyo, 181-8588, Japan

Long duration events (LDE flares) and impulsive flares are defined by duration of X-ray brightening; duration ofLDE flares is typically longer than one hour and duration of impulsive flares is shorter than one hour. Recentspace observations have revealed various evidence of magnetic reconnection and common properties in flares(plasmoid ejection, cusp shaped loops, etc.), leading to unified view of various flares between LDE flares andimpulsive flares. However, the difference between LDE flares and impulsive flares is not well understoodtheoretically. So we examine what makes the difference of duration between LDE flares and impulsive flares byperforming MHD simulation.We assume a octapolar magnetic configuration as an initial condition. Our model is based on the model of Chen &Shibata (2000) and Shiota et al. (2005) which assumes a quadru polar configuration. We add two dipole fields totheir model, in order to regulate the magnetic flux in inflow region and regulate duration and released energy offlare, short duration is the feature of impulsive flare.As a result, it is derived that a difference of magnetic configuration makes the difference between LDE flares andimpulsive flares.

P1-085

Ionospheric Signature of Flow Bursts in the Magnetotail:Geotail-SuperDARN Conjunction StudyTomoaki Hori1, Keisuke Hosokawa2, Yukinaga Miyashita4, Kazuhiro Ohtaka3, Manabu Kunitake3, Shin-ichi Watari3, Takashi Kikuchi1, Yoshifumi Saito4, and Toshifumi Mukai4

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8602, Japan2. University of Electro-Communications, Chofu, Tokyo 182-8585, Japan3. National Institute of Information and Communications Technology, Koganei, Tokyo 184-8795, Japan4. Institute of Space and Astronautical Sciences, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 229-8510,Japan

Ionospheric convection signatures associated with flow bursts in the magnetotail are examined statistically on thebasis of the simultaneous observations made by the Geotail spacecraft and the SuperDARN radars covering thefootprint of Geotail. Our statistical study shows that most (~ 82 %) of the flow bursts in the magnetotail areaccompanied by a significant enhancement of the ionospheric convection flow at the footprint of Geotail mappedalong the field line. Generally the magnetotail flows enhance and decay rapidly, while the correspondingionospheric flows develop as quickly but tend to fade away gradually. However, the start time of most of themagnetotail tail flows coincides with that of the ionospheric flow enhancements within a few minutes. Both thespatial and temporal correspondence suggests that those flow bursts take place as a M-I-coupled process. Whilethe ionospheric convection often shows an overall enhancement of the nightside part of the dawn or duskconvection cell, the most significant enhancement tends to take place at or near the foot point of the correspondingmagnetotail flow bursts. There the ionospheric flow enhancement appears as an uniform convection channel or alocal shear/vortex-like convection cell. Both types of convection enhancement are found with roughly the sameprobability, regardless of the magnetotail flow characteristics. How a flow burst in the magnetotail can have thosedifferent counterparts on the ionospheric side will be discussed by considering substorm effects as well as thespatial characteristics of the flow bursts and the ionosphere.

- 137 -

P1-086

Solar Activity, Different Geomagnetic Storms and Acute MyocardialInfarctions: Results of Collaborative Bulgarian-Azerbaijani StudiesSvetla Dimitrova1, Famil R. Mustafa2, Irina Stoilova1, Elchin S. Babayev2, Katya Georgieva1, Vladimir N. Obridko3, Safura Aliyeva4, and Tatiana Taseva5

1. Solar-Terrestrial Influences Laboratory at the Bulgarian Academy of Sciences2. Shamakhy Astrophysical Observatory (ShAO) named after N.Tusi and Laboratory of Heliobiology, Azerbaijan NationalAcademy of Sciences3. IZMIRAN of Russian Academy of Science, RUSSIA4. Research Institute for Cardiology and Baku city railway policlinic No 2, Ministry of Public Health of the Republic ofAzerbaijan5. University Hospital for Active Treatment St. Anna, Sofia, Bulgaria

Solar activity (SA) has different manifestations: sunspots, solar flares, coronal mass ejections (CME), etc. Twotypes of solar events are the main drivers of geomagnetic activity: CME and mainly their subclass magneticclouds (MC), and high speed solar wind streams (HSSWS) from solar coronal holes. It has been shown that MCand HSSWS have different effects on geomagnetic storms and on the dynamics of the atmosphere. The aim of thepresent collaborative study is to compare their effects on acute myocardial infarct (AMI) occurrence.We used data for the daily distribution of patients who had AMI on the day of admission at the hospital. Theperiod analyzed for Sofia region was from 1.12.1995 to 31.12.2004 and covered 1358 AMI cases, and for grandBaku area 2003-2005 covering 4479 cases.ANOVA was employed to check the significance of the influence of geomagnetic activity and the type ofgeomagnetic storms. Correlation coefficients were also estimated.During maximal SA geomagnetic storms prevail caused by MC, and during minimal SA those caused by HSSWS.The results obtained showed that these two kinds of geomagnetic storms affect in different way the AMIoccurrence. A trend was found (both for the data from Sofia and Baku) for an increase of AMI during stormscaused by MC and a little decrease for the other storms. More investigations are needed to confirm the resultsobtained.

P1-087

Cycles of GCR Diurnal Anisotropy VariationYu Yi and Su Yeon Oh

Department of Astronomy & Space Science, Chungnam National University, Dajeon, Korea

The diurnal variations of GCR intensity observed by the ground NM stations represent the anisotropic GCR flowat 1 AU. It is generally believed that the variation of the local time of the GCR maximum intensity (phase) has22-year period of two sunspot cycles. However, there even exists doubt on such anisotropy variation cycle. Thosedifferent interpretations come from the lack of enough data since determining the cycle of variation in precisionrequires data archived over long time of at least two cycles. In order to determine the cycle of GCR anisotropyvariation, we carried out the statistical study on the diurnal variation of phase. We applied new method indetermining the yearly mean phase. We examined the 52 years data of Huancayo (Haleakala), 38-year data fromRome, 42-year data from Oulu NM stations. We applied the F-test to determine the statistically meaningful periodof anisotropy phase variation. The phase variation has two components of 22-year and 11-year cycles. The NMstation in the high latitude (low cut-off rigidity) shows mainly the 22-year cycle in phase controlled by thediffusion effect with the solar polar magnetic field reversal. However, the lower the latitude of NM station is, thehigher contribution from 11-year cycle associated with the solar sunspot cycle. This additional phase variationmight be regulated by the drift effect.

- 138 -

P1-088

Interaction of Alfven and Slow Magnetosonic WavesEvgeny N. Fedorov, Vyacheslav A. Pilipenko , and Nikolay G. Mazur

Institute of the Physics of the Earth, Moscow, Russia

The interaction of poloidal Alfven waves with slow magnetosonic waves in warm plasmas with the curvilinearitytaken into account is studied theoretically in the linearized 2-D MHD approximation. Dispersion equations fordisturbances with high wave numbers in an axially symmetric finite betta plasma are analyzed. The obtainedsolutions can be applied in the external regions of the Earth's magnetosphere.

P1-089

Relationship between Maximum Number and Fractal Dimension of SunspotNumber in the Solar CycleR.-S. Kim1, Y. Yi1, K.-S. Cho2, Y.-J. Moon2, and S. W. Kim2

1. Chungnam National University, Daejeon 305-764, Korea2. Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea

The fractal dimension is a quantitative parameter describing the characteristics of irregular time series. In thisstudy, we use this parameter to analyze the irregular aspects of solar activity and to predict the maximum sunspotnumber in the following solar cycle by examining time series of the sunspot number. For this, we considered thedaily sunspot number since 1850 from SIDC (Solar Influences Data analysis Center) and then estimated cyclevariation of the fractal dimension by using Higuchi's method. We examined the relationship between this fractaldimension and the maximum monthly sunspot number in each solar cycle. As a result, we found that there is astrong inverse relationship between the fractal dimension and the maximum monthly sunspot number. By usingthis relation we predicted the maximum sunspot number in the solar cycle from the fractal dimension of thesunspot numbers during the solar activity increasing phase. The successful prediction is proven by a goodcorrelation (r=0.89) between the observed and predicted maximum sunspot numbers in the solar cycles.

- 139 -

P1-090

FLR-model Verification Based on the Sunrise-Sunset ULF Geomagnetic FeaturesLeonid Alperovich1, Evgeny Fedorov2, Masashi Hayakawa3, Colin Price1, Moshe Merzer1, Adi Zomer1, and Nadya Yagova2

1. Tel-Aviv University, 69978, Tel-Aviv, Israel2. IFZ RAN, Moscow, Russia3. The University of Electro-Communications, Chofu, Tokyo, Japan

The transition region between dayside and nightside ionospheres is an example of a strong horizontal gradients ofthe electron concentration and as a consequence of this a strong horizontal anomaly of the conductivity exists. Weobtained an explicit solution for the ground magnetic field caused by the Alfven FLR- and FMS-wave incident onthe sunrise-sunset ionosphere. The analytical solutions demonstrate principle distinction in the behavior of theground magnetic field for these two hydromagnetic wave polarizations. We checked dependencies of intensities, orientation angles and polarization of the ULF-geomagnetic oscillationsas a functions of the local time. We used continuous magnetic observations for a few years at Guam, at 4 closeJapanese observatories and at Eilat (Israel). There were revealed two fundamentally different kinds ofgeomagnetic oscillations. The first one is insensitive to the existence of the ionospheric terminator and the otherone is the oscillation behavior of which depends strongly on the ionospheric properties above the observationpoint. It enabled us to consider the first class as the oscillations associated with FMS-hydromagnetic waves andthe cavity magnetospheric resonances. The second class can be rated as Alfven hydromagnetic waves incidentonto the ionosphere. Features of the polarization ellipses and orientation angles near the ionospheric terminatorenabled us to extract a specific geomagnetic pulsation class caused by the FLR hydromagnetic resonances.

P1-091

EM-PIC Simulation Analysis on the Characteristics of Satellite OnboardAntenna in Space PlasmaYohei Miyake, Hideyuki Usui, Hirotsugu Kojima, and Yoshiharu Omura

Research Institute for Sustainable Humanosphere (RISH), Kyoto University

The characteristics of electric field antennas immersed in space plasma are studied by making the most use of theelectromagnetic Particle-In-Cell (EM-PIC) simulations. The antenna is one of the essential instruments for theassessment of the space environment. The accuracy of the measurement depends on the precision of the antennacalibration that is performed based on the antenna properties. However, the properties are affected by complexinteractions among the antenna, plasma waves, and plasma particles. Such effects have to be investigatedquantitatively for the precise calibration of wave electric field data obtained by satellite observations.In the present study, the electric field antenna characteristics are analyzed by self-consistently simulating the fieldevolution and the plasma dynamics in the vicinity of the antenna using the EM-PIC method. To do this, weintroduced the conducting solid surfaces of the antenna or spacecraft bodies as inner boundaries, on which theequipotential solution of electrostatic field is guaranteed. Furthermore, we modeled the interactions between thesolid surfaces and plasma particles considering the body charging effects. Using the method, we revealed that thephotoelectron emission causes the antenna impedance modification in tenuous plasma environment, which is wellrepresented by the RC parallel equivalent electric circuit. We now started the investigation of the characteristics ofan antenna that transmits waves with large amplitude. Such high-power antenna characteristics will be importantfor some experiments such as the control of the radiation-belt electron precipitation by the wave radiation from theantenna.

- 140 -

P1-092

Properties of Coronal Holes Associated with Large Geomagnetic StormsS. Akiyama1, N. Gopalswamy2, and S. Yashiro1

1. The Catholic University of America, Washington, DC 20064, USA2. NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

We studied the characteristics of 11 equatorial coronal holes, which resulted in large (minimum Dst index < -100nT) geomagnetic storms in the interval 1996 to 2004. These storms were part of the Living with a Star (LWS)Coordinated Data-Analysis Workshop (CDAW) in March 2005. We compare comparison between the CH (size,location, magnetic field strength) and the solar wind parameters observed with the Solar Wind Electron, Proton,and Alpha Monitor (SWEPAM) on board the Advanced Composition Explorer (ACE). There were no clearcorrelations except for the relationship between the coronal hole area and the solar wind speed. We estimated theflux expansion rates of CH areas using images obtained by the EUV Imaging Telescope (EIT) on board the Solarand Heliospheric Observatory (SOHO) and the 17 GHz microwave images from the Nobeyama radioheliograph.A slight correlation was seen between the inverse expansion factor and the solar wind speed. We discuss thecoronal hole source and solar wind parameters in understanding the associated geomagnetic storms.

P1-093

Response of the Indian Low Latitude Ionosphere to the Very Large SolarFlare of 28 October 2003 and Associated EffectsG. Manju , Tarun Kumar Pant, C. V. Devasia , and Sudha Ravindran

SPL,VSSC, Trivandrum, India

Using GPS (Global Positioning system) data from stations near the crest of the equatorial ionisation anomaly(EIA) and beyond, ionosonde data and delta_H values at Trivandrum (dip= 0.5 degree), and other low latitudestations, the electrodynamic effects on the low latitude ionospheric regions in the Indian sector have beeninvestigated during the large solar flare (X17.2) of 28 October 2003. The important observations are i) asignificant total electron content (TEC) enhancement (~10 TEC units) at all available GPS observing stationsaround the peak phase of the flare, ii) unusually high h?F values observed at the EIA trough location ofTrivandrum in the late evening hours due to the increased vertical drift, iii) Probable prompt penetration effectsover the Indian regions due to change in polarity of IMF Bz, iv) Absence of enhancement in TEC as seen byionosonde at Delhi during the time of enhanced TEC as seen by GPS is another interesting observation. Theimplications of the observations are discussed.

- 141 -

P1-094

Global Simultaneity of Forbush Decrease EventsSu Yeon Oh and Yu Yi

Department of Astronomy & Space Science, Chungnam National University, Dajeon, Korea

It is generally believed that Forbush Decrease (FD) events happen simultaneously over the globe of the Earth.However, there have been reports on non-simultaneous FD events. We investigate the properties ofnon-simultaneous FD events in order to determine what solar wind conditions lead to global simultaneity of FDevents. We examined the hourly data of the Oulu Neutron Monitor (NM) station from 1997 to 2006. We haveselected 93 FD events that have greater than 3.5 % intensity reductions. Global simultaneity was determined bycomparing the time profiles of these FD events with those recorded by other NM stations at Inuvik and Magadan.Most FD event onsets (62 out of 93) are observed simultaneously by each NM station in universal time (UT)regardless of the location of the NM station, whereas some other FD events are not simultaneously detected, but atsimilar local time (LT). The stronger FD events tend to be simultaneous events, but the weaker FD eventsnon-simultaneous. The latter occurs only if the main phase of the FD is superposed in phase with the decliningphase of diurnal variation, which has the maximum around noon and the minimum around midnight. Thesimultaneous FD events might occur when the high speed strong magnetic barrier (IP shock sheath and MC)overtakes the Earth, whereas the non-simultaneous FD events might occur only when the slow moving weakmagnetic barrier passes by on the dusk side of the Earth. The global simultaneity of FD events depends on speedand IMF strength of solar wind overtaking Earth's magnetosphere and its propagation direction. This model of FDsimultaneity can be tested by the STEREO mission.

P1-095

Rayleigh Lidar Studies of Middle Atmosphere Thermal Structure andDynamics over a Low-latitude Station, Gadanki (13.5 N; 79.2 E)Venkataraman. Sivakumar

National Laser Centre, Council for scientific and Industrial Research (CSIR), P.O. Box 395, Pretoria 0001, South Africa.

In recent years the importance of a systematic monitoring of the temperature structure and dynamics of the lowlatitude middle atmosphere has been demonstrated by several of middle atmospheric programme (MAP)campaigns. A ground based lidar enables the measurement of the temperature profile in the stratospheremesosphere region (30-80 km) with accuracy better than that can be achieved by other groundbased/rocket/satellite techniques. There are large number of studies on middle atmosphere thermal structure have been made for mid- andhigh-latitude stations, but, there were quite limited by number of study on low latitude stratosphere-mesospherethermal structure. A state-of-the-art lidar system has been established in 1998 at National Atmosphere Research Laboratory(formerly known as National MST Radar Facility-NMRF), Gadanki (13.8 N, 79.2 E), India under a joint projectbetween Department of Space, India and Communication Research Laboratory, Ministry of Posts andTelecommunications, Japan. The Indo-Japanese lidar (IJL) comprises of two independent receivers, Rayleigh andMie receivers. Rayleigh backscattering of molecules determines the density and temperature of atmosphere abovethe aerosol layer. It provides consistent measurement of temperature profiles of stratosphere and mesosphereregion (30-90 km) of the atmosphere with accuracy of the order of 1 K. The other, Mie receiver, providesinformation on the aerosol distributions and cloud characteristics over the height range of 06-38 km. The IJL is apolarization diversity lidar which makes it possible to study the thermodynamic phase of the clouds using co- andcross-polarized components. Using Rayleigh lidar measurements made at Gadanki, a detailed study has been made on various aspects of the

- 142 -

low latitude middle atmosphere temperature structure and dynamics. The following are main high-lights of theresults obtained and planed for this presentation.-Middle atmosphere temperature climatology obtained from Lidar, HALOE satellite over the site and itscomparison with different model atmosphere,-Gravity wave studies which includes climatological results, wave breaking region and its saturationcharacteristics,-Studies on planetary and equatorial waves,-Low latitude tides and its short term variations,-Evidence of observed Mesosphere Temperature Inversion (MTI) over a low-latitude,-First results on Sudden Stratosphere Warming (SSW) observed over a low latitude,-First results on observed double stratopause structure over three different northern hemisphere stations, and-Statistical results on sudden stratosphere warming (SSW) observed over three different northern hemispherestations.

P1-096

Global Ionosphere Redistribution due to Strong Geomagnetic Storms (bySatellite Observations)Elvira I. Astafyeva1 and Pavel V. Tatarinov2

1. Department of Natural History Sciences, Hokkaido University, N10 W8 Kita-ku, 060-0810 Sapporo, Japan2. Institute of Solar-Terrestrial Physics, Lermontova str, 126, Irkutsk, 664033, Russia

Magnetic storms represent the largest disturbances in the magnetosphere and ionosphere. After the interplanetarymagnetic field (IMF) turns southward during the main phase of geomagnetic storms, the interplanetary electricfield can penetrate to the low-latitude ionosphere for many hours without decay. The eastward penetration electricfield in the dayside ionosphere moves the equatorial F-region plasma upward enhancing the fountain effect.Here we analyzed ionosphere effects of strongest geomagnetic storms occurred in 2001-2005. For this purpose weused observational data from the CHAMP and SAC-C satellites and from satellite altimeters TOPEX and Jason-1.This allowed us to obtain 3-dimensional visualization of the ionosphere plasma redistribution during stronggeomagnetic storms and to study in detail dayside ionospheric uplift and ionosphere plasma accumulation withinthe crests of the equatorial ionization anomaly (EIA), "gsuper-fountain effect". Besides, use of global ionospheremaps of vertical total electron content (TEC) together with the method of calculation of TEC equal lines seemingdisplacements allowed us to obtain quantitative characteristics of the ionosphere plasma redistribution due togeomagnetic storms. According to our analysis, after Bz of the IMF sharply decreases, TEC value within the EIA area significantlyincreases (up to 180 TEC units by equinox time and up to 120 TEC units by summer time). In a number of eventswe observed poleward traveling of the EIA crests and strong north-south asymmetry. Such asymmetry is causedby neutral wind: the larger plasma flow (toward the hemisphere of stronger poleward wind), the stronger anomalycrest occurs in opposite hemispheres.

- 143 -

P1-097

Comparison of SOHO UVCS and MLSO MK4 DensitiesKyoung-Sun, Lee1, Y.-J. Moon2, Kap-Sung, Kim1, Jin-Yi Lee1, and K.-S. Cho2

1. Department of Astronomy and Space Science, Kyung Hee University, Yongin, Gyunggi, 449-701 Korea2. Korea Astronomy and Space science Institute, Hwaam-dong, Yuseong-gu, Daejeon 305-348, Korea

We have compared the radial density distribution of solar corona obtained by SOHO UltraViolet CoronagraphSpectrometer (UVCS) and Mauna Loa Solar Observatory (MLSO) MK4 coronameter respectively. This is the firstattempt to compare coronal densities obtained by both instruments. In the spectral data of UVCS to examinephysical quantities of corona, we selected two emission lines (O VI 1032A and 1037.6A), which have bothradiative and collisional rate components. The coronal number density was determined from the ratio of these twocomponents. The MK4 coronameter has a field of view ranging between 1.08 and 2.85 solar radii. The coronaldensity could be determined by inverting MLSO MK4 polarization maps. It is found that mean number densitiesof a helmet streamer observed by MK4 at 2003 April 28 are quite consistent with those observed by UVCS. Thisresult demonstrates that MK4 can provide us the coronal density distribution of a large view field with about threeminutes spatial resolution. For the coronal hole and active region observed on 1999 October 19, 23, and 24, theMK4 coronal densities are estimated to be about two times larger than those from the UVCS. For the coronal mass ejection (CME), we determined its electron density and velocity as a function of height. The electron density could be evaluated by the ratio of the forbidden and intercombination lines of O V(1213.8A,1218.4A) and the velocity could be estimated from LASCO and UVCS observations. In addition, we haveinvestigated the height variations of electron density and velocity by using the solar wind model. Results of themodel calculation have been also compared with the observation.

P1-098

Trend Terms in Tropopause and Stratopause Height Time Series at LowLatitude from HALOEShailesh Patel and D. K. Chakrabarty

1. st xavier's college, Navrangpura, Ahmedabad, India2. Center for Environment Survey, Vidyanagar Society, 29/251, Ahmedabad 380 015, India

UAR (Upper Atmosphere Research) satellite has been measuring various parameters since its launch in 1991. Wehave used its temperature data for the period 1991-2005 to examine the trend of tropopause height (TPH) andstratopause height (SPH) at low latitude (23oN, 75oE). Multiple linear regression (MLR) techniques have beenused for the analysis of the quasibiennial oscillation (QBO), seasonal, interannual and solar cycle terms.Considering the whole period of data we find that mean tropopause height is 17.222 km and mean stratopauseheight is 47.550 km. We also find that for tropopause height the value of coefficent of linear trend term is positiveindicating thereby that tropopause is going up over the years. While the value of coefficent of linear trend term isnegative for stratopause height, indicating that stratopause is going down over the years. After applying the abovecorrections, some wave like variation is still seen in the time series.

- 144 -

P1-099

Observation of Daytime Scintillations and its Association with Sporadic-EIrregularities Over Low LatitudeAbhay Kumar Singh1, K. Patel1, R. P. Patel1, and R. P. Singh2

1. Department of Physics, Banaras Hindu University, Varanasi-221005, INDIA2. V.K.S.University, Ara-802301, Bihar, INDIA

The observations of ionospheric scintillation at daytime are attributed to E-region irregularities at high andequatorial latitudes. In this paper, VHF amplitude scintillations recorded during the daytime period from 1991 to1999 at low latitude station Varanasi (geomag. lat. 140 55/ N, long. 1540 E) are analyzed to study the behavior ofsporadic-E irregularities during the active solar and magnetic periods for long terms. It has been found that a highcritical frequency of the Sporadic-E layer are linked with daytime scintillation occurrence.The daytime digital scintillation data have been analyzed to study some important parameters of scintillationproducing sporadic-E irregularities like auto-correlation function, power spectral densities, signal de-correlationtime etc. This paper presents behavior of these parameters under weak and strong scintillation conditions. Resultsof these studies yield important information about the sporadic-E irregularity structures, its shape and size.Derived spectral index ranges between ?2 and ?10 and the characteristics length of sporadic E irregularities variesfrom 100 to 1800 m. The estimated characteristic of these irregularities depends on the velocity and hence weobtain the minimum and maximum range of scale length of sporadic-E irregularities, which were observed overVaranasi. These results are also discussed in the light of recent works.

P1-100

Long-term Changes of the Ionospheric F2-layer Peak Height Deduced fromEISCAT UHF Radar Observations (1984-2004)Tetsuo Motoba1, Yasunobu Ogawa2, Ryoichi Fujii3, and Satonori Nozawa3

1. Graduate school of Environmental Studies, Nagoya Univ.2. National Institute of Polar Research3. Solar-Terrestrial Environment Laboratory, Nagoya Univ.

The EISCAT (European Incoherent SCATter) UHF radar at Tromsoe (69.6N, 19.2E) can provide electron densityprofiles with high temporal and altitude resolution in the auroral ionosphere. A long-time series of the EISCATcommon program 1 (CP1: field-aligned component) data between 1984 and 2004 is used. Since the F2 peakheight (hmF2) observed by EISCAT can directly be estimated without any assumption, the ambiguity fordetecting the real hmF2 is expected to be relatively smaller than that deduced from other ground-basedionospheric instruments, such as the ionosonde. In order to deduce the long-term changes, we need to filter outthe dominating effects from solar activity in the hmF2 variations. In previous long-term trend studies, the F10.7solar radio flux has commonly been used as an index of solar radiation activity. On the other hand, the compositeMg II index is known as a more suitable proxy of the solar extreme ultraviolet (EUV) radiation that ionizes theupper atmosphere, creating the ionosphere. In fact, we find that the observed hmF2 values increase almostlinearly with the Mg II index, while they slightly saturate when the F10.7 index exceeds a threshold(approximately 160-200). In this study, we therefore filter out the dominating effects of solar activity on thehmF2 variation by replacing the F10.7 index with the Mg II index and attempt to derive possible long-termchanges of hmF2 over the last two decades.

- 145 -

P1-101

Climatology of the MesosphereGufran Beig

INDIAN INSTITUTE OF TROPICAL METEOROLOGY, PUNE-411008 INDIA

During the past decade, several attempts have been made to analyze different series of long-term observations andto deduce mesospheric temperature trends. The comparison of the results obtained by different observationsseparated by several decades is complicated. Nevertheless, there are a number of occasions where a majority ofthe temperature trend results indicate consistency and some of the differences are even understandable. There area growing number of experimental results centered on, or consistent with zero temperature trends in themesopause region. The most reliable data sets show no significant trend, but with an uncertainty of at least2K/decade. It is also increasingly clear that until the solar-related changes in the long term temperature series arewell understood and quantified in the mesosphere, there is little hope of separating out changes due to longer-termsecular variability caused due to human induced changes at the surface, much less gaining any insight into theircauses. Present investigations have revealed the presence of a solar component in mesospheric temperature inseveral data sets but not as strong as reported earlier and in some cases no significant solar signal is found. In this talk, an update of the long-term trend and solar signal in temperature of the region from 50-100 km hasbeen made based on available understanding. However, now the major challenge is in the interpretation of thevarious reported results. There appears to be latitudinal as well as seasonal variability in the linear and solartrends. These issues are briefly discussed.

P1-102

Application of 3-D Ionospheric Tomography for Low Latitude RegionsD.Venkata Ratnam1, A.D. Sarma 1, and P.V.D. Somasekhar Rao2

1. R & T Unit for Navigational Electronics, Osmania University, Hyderabad - 500 007, India2. Department of E.C.E, J.N.T University, Hyderabad, India

With the advent of Global Positioning System (GPS), there has been significant improvement in aircraftnavigation. For improving positional accuracy of GPS and for wide coverage, a Satellite Based AugmentationSystem (SBAS) is being developed in India popularly known as GPS Aided Geo Augmented Navigation(GAGAN) system for air-navigation over the Indian service region. As India comes essentially under thelow-latitude region, where the ionospheric behavior is highly dynamic and erratic, the grid based ionosphericmodels suitability is to be investigated thoroughly. The primary tasks in developing an ionospheric model forGAGAN are to consider Total Electron Content (TEC) measurements at fixed reference stations using dualfrequency GPS receivers and combine them in real-time to estimate the current state of the ionosphere. Thepresent paper describes a 3-D model, which is developed on the basis of tomographic techniques. Tomographyrefers to the cross-sectional imaging of an object from either transmission or reflection data collected byilluminating the object from many different directions. In this technique, horizontal direction is defined bySpherical Harmonics Functions (SHF) and vertical direction is defined by Empirical Orthogonal Functions (EOF).The tomographic electron density distribution is obtained using weighted least square method. GPS data collectedfrom 17 GAGAN TEC stations in India are used for the analysis. The developed model is tested using ionosphericstorm data (23 - 25 July 2004). The model reveals that the ionospheric structures during disturbed conditions byestimating accurate delays. The results are compared with 2-D Ionospheric grid models. The standard deviation ofthe 3-D model ionospheric delays is about 1.81 m where as planar fit model standard deviation of ionosphericdelays is about 2.0 m. The mapping error due to slant to vertical TEC and vice-versa conversions can beeliminated using this 3-D model. Hence, the developed tomographic model can be used as one of the key

- 146 -

validation procedures for real time ionospheric delay estimations for GAGAN.

P1-103

Ion Escape Rates from Non-magnetic Earth: On Contribution of TerrestrialIon Flows to Non-solar Components Implanted in Lunar SoilsKanako Seki1, Naoki Terada2, Hiroyuki Shinagawa2, and Minoru Ozima3

1. STEL, Nagoya University, Furocho, Chikusa, Nagoya, Aichi 464-8601, Japan2. NICT, Tokyo 184-8795, Japan3. Graduate School of Earth and Planetary Sci., University of Tokyo, Tokyo 113-0033, Japan

Mechanisms responsible for the atmospheric escape from a planet dramatically change with the strength of itsintrinsic magnetic field. When the planet has substantial global intrinsic magnetic field as in the case of thepresent Earth, the planetary magnetic field provides a barrier against the solar wind and the solar wind cannotblow directly into the upper atmosphere. On the other hand, when the planet has no global intrinsic magnetic fieldas in cases of present Mars and Venus, the solar wind directly interacts with the planetary upper atmosphere andmay cause efficient loss of heavy atmospheric constituents under certain solar wind conditions. The boundary of the solar wind entry for the non-magnetic planets is called the "gionopause". Above theionopause, the terrestrial ions would be accelerated by the electric field induced by the magnetized solar windflow and flow away from the Earth together with the solar wind flow, if the Earth did not posses any intrinsicmagnetic field. This picked-up process can efficiently remove terrestrial ions created above the ionopause. Weestimated the escape rates of each ion species through this escape process using the MSIS00 neutral atmosphericmodel as an input. From the given neutral atmospheric density and temperature, the ion production rate of eachion species is calculated based on previously studies of the photon ionization by solar radiation and photoelectronimpact ionization. Comparison of the result with non-solar ions implanted in lunar soils indicates that theterrestrial ion fluxes from the ancient non-magnetic Earth can be the source of non-solar components of N andlight noble gases implanted in lunar soils [Ozima et al., (2005) Nature, 436, 655-659].

- 147 -

P1-104

Does Sunspot Number Calibration by the Magnetic Needle "Make Sense?"Kalevi Mursula1 and Ilya Usoskin2

1. Dept. of Physical Sciences, University of Oulu, Finland2. Sodankyla Geophysical Observatory, University of Oulu, Finland

It has recently been suggested (Leif Svalgaard, CAWSES Newsletter, 2007) that early sunspot numbers (R) can becalibrated (and significantly corrected) using the geomagnetic inclination range rY. The suggested "correction" is based on a linear regression between rY and R established for the last 25 years. Thisregression "substitutes" R by rY, ignoring the indirect relation between the two variables and their very differentphysical meanings. The suggested "correction" of sunspot numbers by roughly 30% goes far beyond theobservational uncertainties of sunspots, especially in the late XIX century when the Sun was already routinelyobserved by photographic images. We demonstrate that the uncertainties in the past values of rY and in the rY-R regression are, especially due to thearbitrary detrending of the rY series, so large that they smear out the ground for any?gcorrection. We also showthat the relation between rY and R depends on the overall activity level and is nonlinear. This is even expected asrY depends also on the total solar irradiance, not only on UV radiation. Moreover, we note on a differencebetween the long-term behavior of rY and R that needs to be studied as it can lead to a better understanding of theunderlying physics. Thus, the proposed correction hides an interesting problem instead of revealing one, leadingto a loss of valuable information. Concluding, we argue that while the suggested "correction" of sunspot numbers by the geomagnetic inclinationrange makes no sense, the different long-term changes of these two variables should be studied in detail in orderto better understand the different aspects of the Sun-Earth relation.

P1-105

Seasonal Variation of Short-period (<2 h) Gravity Wave Activity overGadanki, India (13.5N, 79.2E)Gopa Dutta1, P. Vinay Kumar1, M.C. Ajay Kumar1, S.P. Alexander2, and T. Tsuda2

1. Anwarul-Uloom College, Osmania University, Hyderabad, India2. Research Institute for sustainable humanosphere(RISH), Japan

We have presente d the seasonal variation of short-period (<2 hour) gravity wave activity in thetroposphere and lower stratosphere (4-21 km) using the wind observations made with VHF radar atGadanki, India. Available wind data collected continuously by the radar for a few hours in a day, with~3 minutes time resolution for four years (2003-2006), have been used for the study of variance andmomentum flux of short-period gravity waves. Both horizontal and vertical variances show annualvariation. Variances in the upper tropospheric and lower stratospheric (UTLS) regions are found tomaximize in the wet season coinciding with the peaks of out going long wave radiation (OLR) andthe rain rate (surface and TRMM 2 km rainfall). Two additional strong peaks of variance areobserved in the height ranges of 4-12 km which correspond to the maxima of TRMM storm heights.The surface wind speed peaks in the wet season and the wind direction is conducive to topographicgeneration of waves. The measurements suggest deep convective activity and topography to beresponsible for the observed nature of variance. An inter-annual variability is observed in themeasured wave activity. Zonal momentum flux shows annual variation with westward preference inthe wet season whereas the meridional flux does not indicate any clear variation. Zonal wind isfound to follow the same trend as momentum flux, particularly in the UTLS region, which needsfurther investigation. The mean drag force per unit mass above 15 km is mostly westward

- 148 -

P1-106

A New Approach to Find Radar Reflectivity vs Rainfall RateRajasri Sen Jaiswal1, S.Uma1, and A. Shanthakumaran2

1. Department of Physics, Sona College of Technology, Salem-636 005, Tamilnadu, India2. Department of Statistics, Sowdeswari College, Salem, Tamilnadu, India

Conventionally a power relation is used globally to estimate rainfall rate from radar reflectivity. Such assumption,however, is questionable as while assuming a power law it has been accepted that rainfall is time independent. Infact rainfall rate is time dependent, i.e., rainfall rate at a particular instant is dependent on that at a previousinstant. In this paper an attempt has been made to find out radar reflectivity versus rainfall rate relationship usingtime series analysis. Ten year disdrometer rainfall rate and reflectivity data over a period of 1998-2007 have beenused for the purpose of this study. The study has been carried over for rainfall rates R

P1-107

Response of Tropical Tropopause to the Heat Transported through Equatorin Indian OceanKrishna Chandra Srivastav1 and I. M. L. Das2

1. M. N. Saha Centre of Space Studies, University of Allahabad, Allahabad - 211002, India2. Department of Physics, University of Allahabad, Allahabad - 211002, India3. K Banerjee Centre of Atmospheric & Ocean Studies, University of Allahabad, Allahabad - 211002, India

There is general agreement that the basic driving force responsible for the variation in tropopause height isvariation in solar radiation at the ocean surface which modulates the sea surface temperature (SST). Thismodulation of SST produces in turn a variation in upper tropospheric potential temperature and hence in theheight and temperature of the tropopause. Several studies have been undertaken to investigate the response oftropical tropopause to variations in SST, in particular to tropical Pacific SST variations.A preliminary work has been undertaken to find the possible relationship between the low latitude tropicaltropopause height and the heat transported through equator in Indian Ocean using Indian MST radar at Gadanki(13.470 N, 79.10 E) and the Chennai (13.100N, 80.200E) radiosonde observations of India MeteorologyDepartment (IMD). A good of correlation of 0.7118 is found between the tropopause heights as measured bychennai radiosonde and heat transported through equator in Indian Ocean. Chennai is a coastal area situated about120 km south - east of the Indian MST radar site at Gadanki. This shows that middle atmosphere dynamics overthe oceanic region / near the coastal area is governed by the changes in the oceanic parameter. When observedwith the radar, we got a very poor correlation of 0.2355 between the estimated tropopause height over Gandankiand the heat transported through equator in Indian Ocean. Gadanki is a land locked area away from the sea. Theresult clearly indicates that height of the tropopause is affected by the orography of the region.

- 149 -

P1-109

Simulation of Surface Heat Budget by RegCM Model in South Asian RegionMd. Mizanur Rahman, Md. Nazrul Islam, and Romee Afroz

1. SAARC Meteorological research Centre (SMRC), Dhaka, Bangladesh2. Plot No. # E-4/C, Agargaon, Dhaka-1207

Regional Climate Model (RegCM3) developed by ICTP, Trieste, Italy is used for simulation of differentmeteorological parameters including net absorbed solar energy flux, net infrared energy flux, sensible heat,evaporation to define Surface heat budget (SHB) over South Asian domain including Bangladesh. The modeldomain is selected to cover the South Asia region (650E-1170E, 50N-350N) on a rotated mercator projection(ROTMER) at a 60 km horizontal grid resolution and 16 sigma levels in the vertical. The centre of the domain is200N, 900E. Daily 6-hour interval Lateral Boundary Conditions (LBCs) data from NCEP is used as the input torun RegCM model and Grell scheme with Arakawa-Schubert (GAS) assumptions is used for validation for theyear 1995-2000 (6-year). It is important to do some validation of the RegCM model outputs to adopt the RegCMfor this region. Due to the lack of surface observational data of SHB over this region, the European Centre forMedium-Range Weather Forecasts (ECMWF) data at 0.50 x 0.50 lat /long (~55 km) horizontal grid resolution isused to calibrate RegCM output. Comparison between model and ECMWF data for SHB has been made in 7selected windows over South Asian region and at the central points of these selected windows for monthly and6-hourly respectively. For the year 1995 the four parameters such as net absorbed solar energy flux, net infraredenergy flux, sensible heat, latent heat of SHB are analysed for the selected domains.The variations of SHB along latitude and longitude have been observed using RegCM model and ECMWF datafor the Pre-monsoon (March-May), Monsoon (June-September) and Post-monsoon (October-November) periods. In general model underestimates SHB from March to May and overestimates from June to September. Over oceanthe value of SHB is high from March to September and low from November to December. On the other hand,over land the same condition is occurred except low in magnitude. SHB at different latitudes along longitudes(700E-940E) is high over ocean and low over land during summer and opposite condition is observed in winter.The difference of SHB between RegCM and ECMWF data are also more over ocean compared to over land. ForSHB the role of latent heat is important for water surface and sensible heat for land surface. According to thediurnal variation of SHB for both RegCM and ECMWF data it has been observed that the peak hour is at 12 LST(local standard time) for GAS.

- 150 -

P1-110

Thermospheric Meridional Winds as Deduced from Meridional IonosondeChain at Low- and Equatorial LatitudesTakashi Maruyama, Masabumi Kawamura, Susumu Saito, Kenro Nozaki, and Mamoru Ishii

National Institute of Information and Communications Technology, 2-1 Nukui-kita 4-chome, Koganei, Tokyo 184-8795, Japan

Multipoint ionosonde observation was conducted in Southeast Asia to study an ionosphere-thermospherecoupling. For this observation three ionosondes were newly installed along the magnetic meridian at 100 deg.E(Southeast Asia Low-latitude Ionospheric Network: SEALION); two of them were a magnetic conjugate pointpair and the other was near the magnetic equator in the same meridian with the conjugate pair. The F layer virtualheight, h'F, was scaled from nighttime ionograms obtained from October 2004 to September 2005. The heightvariations at the three locations were used for deriving thermospheric wind information in the magneticmeridional plane by the assist of model calculations. During the northern winter period, a prominent 6-hr periodicvariation of transequatorial component (with respect to the magnetic equator) was found, while during thenorthern summer period, a diurnal-like variation was dominant. From (northern) winter through summerconditions the dominant component of the periodic variation continuously varied, e.g., an 8-hr variation wasrecognized along with the prevailing southward wind in May and August.

P1-111

Flare and Associated Phenomena in AR 10486 on October 24, 2003Lokesh Bharti, Chandan Joshi, and S.N.A. Jaaffrey

M.L. Sukhadia University, India

Multiwavelength study of flare and associated phenomena in AR 10486 is presented. Surges observed after flarepeak time. RHESSI data shows upward moving source in 3-12 keV band. Bright mass ejection seen in TRACE1600 images well correlated with this upward moving source. Observations of TRACE 195 reveals that the surgeejected from foot point of a flaring coronal loop. Magnetic reconnection may be plausible mechanism to supplysufficient energy for surges and coronal loop heating.

- 151 -

P1-112

Streamer Belt and Chains as the Main Sources of Quasi-stationary SlowSolar WindM. Eselevich1, V. Eselevich1, and K. Fujiki2

1. Institute of Solar-Terrestrial physics, Irkutsk, Russia2. Solar-Terrestrial Environment Laboratory, Nagoya University, Toyokawa, Japan

It has been known that periods of the low geomagnetic activity in near-earth environment coincide with arrivaltime of the "slow" solar wind (SW) at Earth's orbit. In this connection, sources of the "slow" SW on the Sun aresignificant issue in the space weather problem. In this work synoptic maps of white-light coronal brightness fromSOHO/LASCO C2 and distributions of solar wind velocity obtained from interplanetary scintillation were studied.Regions with velocity V = 300-450 km/s and increased density N > 10 cm^(-3), typical of the "slow" solar windoriginating from the belt and chains of streamers, are shown to exist at Earth's orbit, between the fast solar windflows (with a maximum velocity Vmax = 450-800 km/s). The belt and chains of streamers are the main sources ofthe "slow" solar wind. As the sources of "slow" solar wind, the contribution from the chains of streamers may becomparable to that from the streamer belt.

P1-113

Trying to Understand Solar Luminosity Variations with the Virial TheoremAntonio Ferriz-Mas1 and Oskar Steiner3

1. Departamento de Fisica Aplicada Facultad de Ciencias de Orense Universidad de Vigo E-32004 Orense, Spain2. Department of Earth and Planetary Science University of Tokyo Tokyo 113-0033, Japan3. Kiepenheuer-Institut fur Sonnenphysik Schoneckstr. 6 D-79104 Freiburg, Germany

The variability of solar radiance over a solar cycle is probably the result of a delicate balance between theradiative deficit of sunspots and the extra contribution of plage and network regions: Sunspots are cooler than thesurrounding photosphere and block part of the outgoing radiation. On the other hand, faculae are magnetic fluxbundles that lead to a depression of the solar surface at their location; in regions where they are abundant (plageand network), they increase the "roughness" of the solar surface, thus increasing the effective surface from whereradiation can escape.While Spiegel & Weiss (1981) suggested that the cause of luminosity variations was in the magnetic field at thebase of the solar convection zone, conventional wisdom nowadays is that it is the direct result of surfacemagnetism. In this contribution we try to show how solar luminosity variability might be connected to a deeplyseated flux-tube dynamo and how the connection with the surface is established on a hydrodynamical time scale.We make use of the virial theorem for a continuum (Chandrasekhar & Fermi, 1953), which is basically a globalstatement of momentum balance. Some energy estimates are considered. The physical picture underlying ourapproach is that the toroidal flux system responsible for the sunspot cycle is stored in the form of flux tubes withfield strength close to 10^5 Gauss at the bottom of the solar convection zone. The process of flux-tube rise andflux-tube explosion can be interpreted as a magnetoconvective mixing-length transport, similar to, but moreefficient than the regular hydrodynamic convection. By this process, the convection zone can find a more efficientmeans of transporting energy across it, limited only by the number of available magnetic flux tubes.

- 152 -

P1-114

Statistical Study of Chromospheric Anemone Jets Observed withHinode/SOTTahei Nakamura1, Naoto Nishizuka1, Tomoko Kawate1, Kazunari Shibata1, Takuma Matsumoto1, Kenichi Otsuji1, Shin'ichi Nagata1, Satoru UeNo1, Reizaburo Kitai1, Saku Tsuneta2, Yoshinori Suematsu2, Kiyoshi Ichimoto2, Toshifumi Shimizu3, Yukio Katsukawa2, and Kazunari Shibata1

1. Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471, Japan2. National Astronomical Observatory, Mitaka, Tokyo 181, Japan3. Institute of Space and Astronautical Science JAXA

Solar Optical Telescope (SOT) aboard Hinode (Solar B) discovered numeroustiny jets in the chromosphereoutside sunspots with Ca II H broad band filter. Typical Ca jets have cusp structure at the footpoints, similar tothe shape of X-ray anemone jets observed with Yohkoh soft X-ray telescope in the 1990s, although the size of Cajet is about 1/100 that of X-ray jet. We think Ca jets are small scale version of X-ray anemone jets, and may becalled chromospheric anemone jets or simply Ca jets.To study origin of Ca jets, we examined jets in solar active region near solar limb, because the structures of Cajets were clear near solar limb. We studied Ca jets statistically and found following characteristics. Typicallength of Ca jets is 1000-10000km, width is 100-300km, cusp size is 1000km, lifetime is 100-1000s, and velocityis 10-20km/s.The velocity of jets is comparable to local Alfven speed in the low chromosphere and structures are similar tothose of X-ray anemone jets, so it is suggested that Ca jets are produced by magnetic reconnection between smallbipole (tiny emerging flux ?) and pre-existing (locally uniform) magnetic field in the low chromosphere. There isalso some evidence that there are mixed magnetic properties at the footpoints of Ca jets, supporting magneticreconnection model.

- 153 -

P3-001

Local Linear Growth Rate of Collisional Rayleigh-Taylor Instability underGeomagnetic Disturbed Conditions during Solar MaximumChien-Chih Lee

General Education Center, Ching-Yun University, Jhongli City, Taoyuan County, Taiwan

This study chooses 5 cases under geomagnetic disturbed conditions to investigate the effects of geomagneticdisturbance on local linear growth rate of collisional Rayleigh-Taylor (CR-T) instability. In the case at 30 July1999, the growth rate at 1900 LT is larger than the monthly averages of April and October 1999. Since theoccurrences of equatorial spread F (ESF) are higher in April and October, the ESF is generated in the sunsetperiod. In contrast, at 12 and 22 September 1999, the growth rate at 1900 LT is smaller than the associatedmonthly average of June 1999, in which the ESF occurrence probability is lower. Thus, the ESF does not occur inthese two days. In addition, the growth rates in the cases of 26 September and 31 December 1999 are not affectedby the geomagnetic disturbances. The ESF appear in these two days, because of the higher ESF occurrences inSeptember and December. These results show that the geomagnetic disturbance can be an important but variablefactor for changes to the local linear growth rate of CR-T instability that controls the development of ESF.

P3-002

Neural Network Prediction of Solar Wind Velocity by Objects on the SunImagesJulia S. Shugai, Sergey A. Dolenko, Igor G. Persiantsev , and Igor S. Veselovsky

Institute of Nuclear Physics, Moscow State University, 119992, Moscow, Russia

We present a hierarchical neural network algorithm for prediction of the daily values of the solar wind velocity bythe areas of low-latitude coronal holes and active regions, and mean magnetic field of the Sun. These areas wereobtained by processing daily snapshots of the Sun, made by the telescope EIT/SOHO at 28.4 nm wavelength for1999 - 2006 years. The neural network predictions were compared to the observed values of the solar windvelocity. The model predicted the solar wind velocity at Earth's orbit for 2005 year with 13% average relativeerror and linear correlation coefficient equal to 0.6. A significant feature of the used approach is the possibility ofsearch for non-linear interconnections between the parameters of the objects on the Sun images and the values ofsolar wind velocity. The algorithm was capable to estimate the delay between observation of a coronal holesregion at the Sun and strong variations of the solar wind velocity observed at Earth's orbit.

- 154 -

P3-003

On Monthly/Seasonal/Longitudinal Variations of Equatorial IrregularityOccurrences and Their Relationship to Post-Sunset Vertical Drift VelocitiesShin-Yi Su1, Chi-Kwan Chao2, and Chao-Han Liu3

1. Institute of Space Science, and Center for Space and Remote Sensing Research, National Central University, Chung-Li,Taiwan.2. Institute of Space Science, National Central University, Chung-Li, Taiwan.3. Academia Sinica, Taipei, Taiwan.

Global monthly variation of equatorial density irregularity distribution has been obtained with data taken byROCSAT-1 at the 600 km topside ionosphere from March 1999 to June 2004 during high to moderate solaractivity periods. This global longitudinal distribution of monthly density irregularity occurrence variation notonly provides the best spatial/temporal distribution existed so far but also fills the large gap of irregularitydistribution missing over some Pacific regions where no ground observation is available. The 5½-year result ofthe monthly occurrence pattern indicates a smooth variation across longitudes contrary to some beliefs that adrastic change in irregularity occurrence pattern can occur across some longitudes in the Pacific. Excellentagreement is noted for the current results with Aarons' conjectured sketch of global scintillation occurrencedistributions published in 1993. Furthermore, the seasonal/longitudinal (s/l) variations of quiettime post-sunsetvertical drift velocities are found to track closely with the s/l variations of irregularity occurrences except duringthe September equinox season. Linear regression analysis between the vertical drift velocity and the irregularityoccurrence rate has been carried out to study the correlation between the two for seasonal as well as longitudinalvariation. The results indicate that the vertical drift velocities at three different longitude zones of differentmagnetic declinations have good correlations with irregularity occurrences for all seasons. This implies that theaveraged post-sunset vertical drift velocity is indeed a good indicator for the occurrences of equatorial densityirregularities in a longitude region of same magnetic declination. In other words, the post-sunset vertical driftvelocity can drive the equatorial occurrence in proportion even though its effectiveness has longitudinal variation. The most effective longitude is in the South America-Atlantic region, while the worst one is in the Pacific regionwhere some large perturbation seeds seem needed to assist the occurrences of irregularities.

- 155 -

P3-004

Plasma Stresses at Equatorial Plane Developed by Slow Mode Waves as aPrimary Acceleration of AuroraOsuke Saka1 and Kanji Hayashi2

1. Office Geophysik, , Ogoori 1165-1, 838-0141, Japan2. Department of Earth and Planetary Science, University of Tokyo, Japan (retired)

Surface waves in the midnight magnetosphere are classified as Pi2 band oscillations and they are triggered at theequatorial plane by plasma injections during substorm expansion onset [Saka et al., 2007]. Plasma compressionsand decompressions by surface waves may generate locally a minimum field strength region (minimum B) in theequatorial plane of injected plasmas. The field-aligned stresses would be developed in the equatorial plane byslow mode waves at the minimum B by the combined effects of magnetic mirror force and field-aligned gradientof plasma pressures [Saka et al., 2005; Saka, 2006]. From detailed analyses of the auroral event of January 241986 using all-sky TV images and magnetometer data from geosynchronous satellites, we have ascertained thatauroras are ignited repeatedly at Pi2 band frequencies during the interval when the field-aligned stresses wereintensified at the equator. To account for the correlation between stresses in the equatorial plane and auroraignition, we argue that slow shocks launched from the minimum B may release the stresses therein by thetransport of plasma sheet materials in the injected plasmas to the particle acceleration regions in lower altitudes.

References[1] O.Saka, S.Fujita, and D.N.Baker (2005), Adv.Polar Upper Atmos.Res. 19, 84-88.[2] O.Saka (2006), Adv.Polar Upper Atmos.Res., 20, 38-45.[3] O.Saka, D.Koga, and K.Hayashi (2007), J.Atmos.Solar-Terr.Phys., 69, 1063-1074.

P3-005

Study of Earthward Flow Burst and Bursty Bulk Flow in the Near-EarthGeomagnetotail by Three Dimensional MHD SimulationKoji Kondoh and Masayuki Ugai

Dept. of Computer Science, Ehime University, Japan

We examine the short-term fast flow event (Flow Burst) and the long-term fast flow event (Bursty Bulk Flow)which are observed in the near-Earth geomagnetotail plasma sheet using three dimensional MHD simulation. This study is based on the idea that these fast flow events are caused by the fast magnetic reconnection. And, thespontaneous fast reconnection model is employed to these simulations. In the previous study, we showed thatin-situ observation results, the profile of quantities, are quite different in each satellite position relative to theX-point and the reconnection jet. In this study, we'll show the effects of the multi-X-points to the profile ofquantities detected by the in-situ satellites and explain the differences between FB and BBF by them.

- 156 -

P3-006

Space Weather Modeling on the Solar Flare Event in December 2006 (2):From Interplanetary Space to EarthT. Ogino1, R. Kataoka2, T. Obara3, Y. Omura4, K. Kusano5, K. Shibata6, and the Modeling Task Force Group

1. Solar-Terrestrial Environment Laboratory, Nagoya University2. The Institute of Physics and Chemical Research, Saitama, Japan3. National Institute of Information and Communications Technology, Japan4. Research Institute for Sustainable Humanosphere, Japan5. The Earth Simulator Center, Japan Agency for Marine-Earth Science and Technology, Japan6. Kwasan Observatory, Kyoto University, Kyoto, Japan

One of the important issues on space weather study is to make a physical model and to simulate a series ofphenomena from origins of disturbances in the sun to the responses of magnetosphere and ionosphere in earth.Under the Creative Scientific Research "The Basic Study of Space Weather Prediction", we have firstly tried sucha series of modeling on the solar flare event in December 13-16 2006 and the geomagnetic storms. Following thespace weather modeling (1) from the sun to solar wind, we present the space weather modeling (2) from the solarwind to the magnetosphere-ionosphere response in the earth. Large interplanetary disturbances were generated inassociation with the strong solar activity of X-class flares on 12/13 and 12/14. Propagation of the disturbancesfrom the sun to the earth is simulated by using 3D global solar wind model following evolution of solardisturbances. A 3D global MHD simulation of interaction between the solar wind and earth's magnetosphere iscarried out by using the output of the 3D solar wind simulation. Moreover, magnetosphere-ionosphere coupling,ionosphere convection in the polar region, energetic particles in radiation belts and precipitation of energeticparticles due to wave-particle interaction are discussed in association with geomagnetic storms generated by thesolar flare event.

P3-007

Global Ionospheric Weather Observed by the FORMOSAT-3/COSMIC:Seasonal Effects and Atmosphere-Ionosphere CouplingCharles Lin1, Jann-Yenq (Tiger) Liu, and Chao-Han Liu

1. National Space Organization, Hsinchu, Taiwan2. Institute of Space Science, National Central University, Chung-Li, Taiwan3. Academia Sinica, Taipei, Taiwan

The new era of studying the ionospheric space weather effects has come after the launch of the innovative satelliteconstellation, named as FORMOSAT-3/COSMIC (F3/C), performing radio occultation experiment capable ofobserving global ionosphere three-dimensionally. This is the first time that a satellite constellation providesinstantly both the lower and upper parts of the ionospheric electron density up to the altitude of the satellites. With more than 2500 soundings of the ionospheric vertical electron density profiles every day, ionospheric plasmastructures over many continents and most of oceans, where ground-based observation is limited, are now observedcontinuously. Important ionospheric research topics, such as space weather effects to the ionosphere, variations ofionospheric plasma structure and dynamics produced by solar outputs, and atmosphere-ionosphere couplingprocesses, can be widely studied and modeled based on the three-dimensional ionospheric images constructed bythe F3/C observations. After one year in orbit, great amount of radio occultation soundings allow us to constructglobal ionospheric maps to study the ionospheric seasonal effects and the atmosphere-ionosphere interactions. Taking advantage of the uniqueness of the dense global coverage, the major physical mechanisms of the twostudies are given. Additionally, horizontal total electron content (TEC) between GPS satellite and F3/Cmicrosatellite is combined with a network of ground-based GPS receivers to perform the ionospheric tomography. Horizontal TECs between GPS satellite and F3/C microsatellite helps to regularize undetermined tomographicinversion problem and gives more information on vertical electron density distribution. Example of reconstructedionospheric images is also presented to show the potential application.

- 157 -

P3-008

Substorm Occurrences during HILDCAA IntervalsHee-Jeong Kim1 and Dae-Young Lee2

1. Department of Astronomy and Space Science, Kyung-Hee University, Yongin 446-701, Korea2. Department of Astronomy and Space Science, Chungbuk National University, Cungju 361-763, Korea

Examination of interplanetary magnetic field data shows that the large amplitude Alfenic fluctuations can appearfor slow speed streams (Vsw < 600 km/s) as well as for high speed solar wind streams. One can identify so-calledHILDCAA (High-Intensity Long-Duration Continuous AE Activity) events from IMF Bz and Dst variationswithout invoking AE index. A prolonged interval of sustained large amplitude Alfvenic waves in IMF Bz and more or less constant small decreases in Dst ( > ~ -50 nT) results in a HILDCAA event. We have analyzed solarwind and magnetospheric parameters to study the relationship between substorm occurrences and HILDCAAevents. Examination of LANL low energy (~10s-100s keV) electron fluxes and IMAGE aurora data show thatrepetitively occurring particle injections during HILDCAA intervals are highly correlated with auroral substorms.

P3-009

Space Weather Influence on Meteor FluxThomas Djamaluddin

National Institute of Aeronautics and Space (LAPAN), Bandung 40173, Indonesia

Meteor Wind Radar installed at Kototabang Aerospace Observatory (0.20 S, 100.32 E), under Japan (KyotoUniversity) - Indonesia (LAPAN) collaboration research program, provide continuous data of meteor flux. Itsvariation is dominated by ecliptic variation. However, there is also solar activity influence indicated from dailyvariation of the flux. This preliminary result indicates that meteor flux variation may not be due to atmosphericresponse to space weather, but to interplanetary dust response.

- 158 -

P3-011

Latitude and Local Time Dependences of Ionospheric Currents During aGeomagnetic StormYuji Tsuji, Atsuki Shinbori, and Takashi Kikuchi

Solar-Terrestrial Environment Laboratory, Nagoya University

In order to clarify the distribution of electric field and current in the middle- and low-latitude ionosphere during ageomagnetic storm, we analyzed ground magnetic disturbances for the geomagnetic storm on September 7, 2002with the minimum SYM-H value of -168 [nT]. In this analysis, we investigate magnetic field deviations of the Xcomponent from the SYM-H value as functions of the magnetic latitude and local time. The magnetic deviation atthe low latitude was positive and negative in the dawn and dusk sectors, respectively, during the main phase of thestorm. This tendency represents a remarkable dawn-dusk asymmetry in the storm-time ring current. On the otherhand, the magnetic deviation at the middle latitude was negative and positive in the morning and afternoonsectors, respectively. This local time tendency coincides with that of the DP2 currents. When the interplanetarymagnetic field turned northward, the storm turned into the recovery phase. We found that the magnetic deviationat the middle latitudes in the early recovery phase was in opposite sense to that of the magnetic deviation duringthe storm main phase. This implies that the overshielding took place at the middle latitudes, due to an abruptdecrease of the convection electric field. This result suggests that the electric field reversed its direction in theinner magnetosphere during this phase. During the late recovery phase, the dawn-dusk asymmetry both at themiddle and low latitudes became weak in all magnetic local time because of symmetrized ring current.

P3-012

Numerical Reconstruction of Three-Dimensional Solar Coronal MagneticField Based on Photospheric Magnetogram DataS.Inoue1, K.Kusano2, S.Masuda1, T.Miyoshi3, T.Magara4, T.Yamamoto4, S.Tsuneta4, T.Sakurai4, T.Yokoyama5, and Hinode/SOT team

1. STEL/Nagoya Univ.2. ESC/JAMSTEC3. Hiroshima Univ.4. NAOJ5. Univ. of Tokyo

The solar active phenomena, such as solar flares and coronal mass ejections (CMEs), are widely believed to be asudden release of magnetic energy stored in the solar corona. Therefore, the three-dimensional structure of coronalmagnetic field is very important to reveal their trigger mechanism as well as to predict the onset of solar weatherevents, although the trigger process is not yet well understood. The coronal magnetic field can be well approximated by force-free field, because plasma beta value is muchsmaller than unity in the solar corona, and thus the extrapolation of the force-free field based on vectormagnetograms must be a promising method to understand the magnetic structure. However, since the force-freefield equation is nonlinear in general, it is impractical to solve that analytically, and thus the efficient numericalsolver of the nonlinear force-free (NLFF) field has been highly required. In this study, we have developed a new NLFF field solver, in which the conventional magnetofrictional method isextended by adapting a multi-grid technique and the optimized searching procedure of initial trial function. First,we have examined the accuracy and the reliability of this new method by comparing the numerical results with thesemi-analytical solution introduced by Low & Lou (1990). Second, we have applied the new solver onto a seriesof magnetograms for active region NOAA10930, which were observed by HINODE/SOT during the pre-flare andpost-flare phases of an X-class flare on Dec. 13, 2006. Based on the result, we will discuss the evolution of

- 159 -

magnetic energy and helicity during the flaring process. The result indicates that the magnetic helicity is about0.046Phi^2, where Phi is the total magnetic flux across the active region.

P3-013

Influence of Plasma Sheet Density, Temperature and Local TimeDistribution on Proton Ring Current Strength and MorphologyBenoit Lavraud, Vania K. Jordanova, and Michelle F. Thomsen

Space Science and Applications, Los Alamos National Laboratory, 87545 Los Alamos, New Mexico, USA

The ring current strongly depends upon the properties of the plasma injected from the magnetotail. The presentwork is motivated by the knowledge that this typically hot and tenuous plasma can, at times, (1) be substantiallycolder and denser, and (2) be injected at varying local times, with recent observations suggesting a cold-denseplasma source at dawn of geosynchronous orbit during storms. We have run a kinetic model of the ring currentwith different plasma sheet boundary conditions to test the systematic influence of these varying conditions on thering current strength and morphology. We show in particular that a cold-dense plasma sheet is more geo-effectivethan a hot-tenuous one, as has been suggested by observations, and that the local time distribution of the injectedplasma is of prime importance, in particular for its morphology. While cold and dense plasma may convect deepinside the ring current region, hotter plasma is more subject to magnetic drifts and quickly drifts toward dusk withlower energization. These modeling results illustrate how both the presence and location of cold-dense plasmasources in the magnetotail influence the ring current during an ensuing storm.

- 160 -

P3-014

Geomagnetic Storms and Their Local Time Dependant Effects on GlobalEquatorial and Low Latitude SectorsD.S.V.V.D. Prasad, S. Tulasi Ram, S. Gopi Krishna, P.V.S. Rama Rao, and K. Niranjan

Space Physics Laboratories, Department of Physics, Andhra University, Visakhapatnam, India

The ionospheric electric fields and currents at equatorial and low latitudes during disturbed geomagnetic activityperiods differ significantly from their quiet-day patterns due to the high latitude &#8211; low latitudeelectro-dynamical coupling and the dynamic interaction between ionosphere-thermosphere-magnetospheresystems. This paper presents a comprehensive study carried out on Geo-magnetic storm time variations in TEC,Equatorial Ionization Anomaly (EIA), and scintillations at VHF and L-band frequencies over Indian sector duringthe low and descending phase of the solar cycle epoch (2004-2006) using Indian GPS receiver network data (18stations) under ISRO-GAGAN project along with simultaneous observations of VHF and L-band scintillationsfrom two-geostationary satellites (FLEETSAT (73 deg E) and INMARSAT (65 deg E)) over a low latitudestation, Waltair (17.7 deg N, 83.3 deg E), India. A detailed study carried out on five moderate to intense geomagnetic storms during 2004 to 2006 has revealed thatsignificant enhancements as well as reversals in ElectroJet current and a corresponding intensification anddiminution of Equatorial Ionization Anomaly (EIA) is observed in a highly local time (longitude) dependantmanner. Large post sunset vertical drifts followed by occurrence of intense SpF, scintillations at 250 MHz and1.5 GHz frequencies have been repeatedly observed when there is a rapid decrease in the Dst/Sym-H index (>15nT/hr) around local sunset hours. Further, the Sp-F, VHF and L-band scintillations continued to occur forlonger durations extending up to post-midnight to pre-dawn hours possibly due to the combined effects of promptpenetration and disturbance dynamo electric fields associated with geomagnetic storm activity. Also, strongreversal in Electrojet currents, significant reduction in EIA strength, suppression of PRE ExB drift and subsequentinhibition of Sp-F and scintillations were observed when a rapid decrease in Dst/Sym-H index occurs around noonhours. Further, the close association observed between the day time EIA strength and the post sunset verticaldrifts at the equator and the role of these two parameters in forecasting the onset of scintillations over equatorialand low latitudes has also been discussed in this paper

- 161 -

P3-015

Radial Diffusion Coefficients for Inner Part of the Radiation BeltKengo Komatsu1 and Shigeto Watanabe2

1. Division of Earth and Planetary Science, Graduate School of Science, Hokkaido University, N10W8, Sapporo, Japan2. Division of Cosmosciences, Graduate School of Science, Hokkaido University, N10W8, Sapporo, Japan

A radial diffusion model can reproduce a basic structure of the radiation belts [Lyons and Thorne, 1973].Radiation belt particles are supplied from the plasmasheet, and the flux is arranged by the balance of intensity ofthe diffusion and the loss due to pitch-angle scattering. However it has been thought that additional heatingprocesses are needed in the outer belt because a negative gradient of the phase space density in the outer beltduring a recovery phase of magnetic storms could not reproduce by only the radial diffusion.Radial diffusion coefficients formulated by Brautigam and Albert [2000] are customarily used in thetime-dependent radial diffusion model. They parameterised electric field variations as a linear function of Kpindex, and applied them to the electrostatic coefficient derived by Cornwall [1968]. They were also formulated theelectromagnetic coefficient as the function of Kp index. Because these coefficients are based on the observation ofthe outer belt, it is not appropriate to apply them to the slot and the inner belt regions. In fact, extrapolating thesediffusion coefficients to the slot and the inner belt and doing numerical simulation, the slot is not formed and theflux near the Earth region is too large.In this study, we assumed that diffusion coefficients become smaller drastically in the plasmasphere. The modelwith such diffusion coefficients forms the slot and the inner belt and also reproduces the negative gradient of thephase space density in the outer belt without additional heating processes.

P3-016

Variation of the Cold Plasma Density Structure above the Polar IonosphereAssociated with Geomagnetic StormsNaritoshi Kitamura1, Atsuki Shinbori2, Yukitoshi Nishimura1, Takayuki Ono1, Masahide Iizima1, and Atsushi Kumamoto1

1. Geophysical institute, Tohoku University, 6-3 Aramaki, Azaaoba, Aoba-ku, Sendai, 980-8578, Japan2. Solar-Terrestrial Environment Laboratory, Nagoya University, Furoucho, Chikusa-ku, Nagoya, 464-8601, Japan

Plasma outflow from the polar ionosphere is one of the most important magnetosphere-ionosphere couplingprocesses in the polar region. In order to clarify the physical process of an abrupt change of the plasma densityfound in the high altitude polar ionosphere during geomagnetic storms, we analyzed the electron density dataobserved by the Akebono satellite in an altitude range from 300 to 10500 km.First, we analyzed storm time data of June 6, and June 9, in 1989 when the satellite located above the southernhemisphere. In these events, plasma density enhancements were clearly associated with the storm main phases. Inthe June 6 storm, the electron density enhanced up to 100 times as large as the average density measured duringmagnetically quiet times in winter season.Using the data from March, 1989 to July, 1990 we performed statistical analyses of the electron density. Theseelectron density data were sorted into two geomagnetic conditions. They are magnetically quiet condition andstorm main phase period based on SYM-H and Kp indices. During the main phase, the electron density increased3 (in summer) to 10 (in winter) times compared with the quiet-time distribution in the altitude range from 3000 to10500 km and invariant latitudes higher than 65-70 degrees.It is concluded that a large amount of the ionospheric plasma is transferred to the region of 10000 km altitude inthe magnetosphere associated with the geomagnetic storms.

- 162 -

P3-017

Role of Solar Wind Magnetic Field in the SC-Triggered SubstormKenichi Kudo, Takashi Kikuchi, and Atsuki Shinbori

Solar-Terrestorial Environment Laboratory, Nagoya University, Aichi, Japan

Numerous works showed the substorm was triggered by sudden commencements (SCs) produced byinterplanetary shocks. In this work, classifying IMF associated with solar wind shock into three types, weexamined the response of the magnetosphere. These three types are characterized by; (1) negative Bz at the shockfollowed by northward turning within 10minutes, (2) negative Bz at the shock followed by enhanced negative Bz,(3) positive Bz followed by enhanced positive Bz. It was found that the type-1 condition most probably triggeredthe substorm. For instance, SC triggered substorm at 0:46UT in April 18, 2001 was typically triggered by type-1condition. SC was observed at 0:46:30UT in Kakioka station, thereafter at 0:54 aurora breakup was observed byIMAGE FUV. At 0:54, aurora expanded azimuthally, thereafter expanded poleward. Also, at 0:54 energeticparticle was injected at midnight in geosynchronous orbit and thereafter negative bay was observed at the groundmagnetometer. Therefore, substorm onset was determined at 0:54. Focusing on the time of about 8 minutes afterSC, we compared this time lag with the time interval between the shock front and the northward turning. As aresult, we noticed that the substorm onset time mostly corresponds to the northward turning. Also, we statisticallyexamined 13 substorm by type-1 condition. As a result, we found that the time interval between the shock frontand the northward turning in the type-1 corresponds to the time delay between the SC onset and substormexpansion onset. It is suggested that the time lag of the onset of the substorm from the solar wind shock is due tothe time lag of the northward turning of the IMF. Researching substorm by IP shock is advantageous in clarifying whether northward turning triggers substormexpansion or not. Substorm expansion onset is determined by using IMAGE FUV/WIC, ground magnetometerand so on, we show that how the aurora and the ground magnetometer varies during northward turning in IMF Bz.

P3-018

Space Weather Signatures of Interplanetary Shocks Associated With CME,CH and MC During 2005Girija Rajaram1, Radharani Alyana1, Jatin Rathod1, D.S. Misra1, C.G. Patil2, and M.Y.S. Prasad3

1. ISTEC-B, CSRE, IIT-B, Powai, MUMBAI-400 076, INDIA2. MCF-ISRO, PB No 66, HASSAN-573201, Karnataka State, INDIA3. DECU, SITAA-SAC, ISRO, AHMEDABAD-380015, Gujarat State, INDIA

CME (Coronal Mass Ejection), CH (Coronal Holes) and MC (Magnetic Clouds) are energetic to very energeticSolar phenomena which cause considerable Space Weather disturbance in the Interplanetary medium and inGeospace. During such events, Satellites at the dayside Lagrangian point L1 record Shock structures in allparameters of the Solar wind and the Interplanetary Magnetic Field, but the nature of the structures differsbetween the three.Such events also disturb the flux densities of relativistic 2 MeV electrons and 1 - 5 MeV and 10 - 30 MeV protonsat Geostationary orbit (GSO), and this aspect assumes importance in causing operational anomalies in spacecraftlocated at this orbit. We try to relate the egeoeffectiveness of the fluence of the 2 MeV electrons to the nature ofthe Shock associated with the CME, CH and MC events. Changes in electromagnetic conditions innear-Geospace (i.e. the Ionosphere and the Inner magnetosphere) associated with these events reflect as sharpvariations in the geomagnetic indices Dst and Kp, and the Cosmic Ray Neutron Monitor (CRNM) Count at Earthis also seen to show sharp Forbush-like decreases.In this work, 8 CME, 4 CH, and 3 MC events which occurred during 2005 are studied for their Space Weathereffects at the L1 point, the Geostationary orbit and at Earth. We try to relate the differences in effects between the3 Categories, to the type and nature of the Shock observed at the L1 point.

- 163 -

P3-019

A New Magnetometer Array in Southeast Europe for Space WeatherMonitoringIoannis A. Daglis1, G. Balasis1, P. Kapiris3, B. Di Fiore1, W. Baumjohann2, W. Magnes2, A. Anastasiadis1, and M. Georgiou3

1. National Observatory of Athens, Institute for Space Applications and Remote Sensing, GR-15236 Penteli, Greece2. Space Research Institute, Austrian Academy of Sciences, Graz, Austria3. Department of Physics, National University of Athens, Zografos, Greece

The National Observatory of Athens is currently setting up a magnetometer array in Greece, in collaboration withthe Austrian Academy of Sciences. The magnetometers will be providing measurements primarily for the study ofgeomagnetic pulsations, resulting from solar wind - magnetosphere coupling. The array will eventually consist of4 stations latitudinally equi-spaced between 37deg and 42deg N geographic latitude. The particular spatialconfiguration is suitable for detecting field-line resonance signatures, thus allowing the study of the dynamics ofthe inner magnetosphere. Field line resonance frequencies can be accurately determined by means of across-phase analysis of ground-based ULF wave measurements recorded at stations closely spaced in latitude.This enables monitoring of the temporal variations of the plasma mass density in the inner magnetosphere, whichis a critical parameter in geospace storms dynamics and space weather dynamics in general. The new array willprovide the potential for collaboration with the South European GeoMagnetic Array (SEGMA) and with arrays inother parts of the globe for a more efficient and comprehensive space weather monitoring and nowcasting.

P3-020

Vlasov Code SimulationsTakayuki Umeda

Solar-Terrestrial Environment Laboratory, Nagoya University, Aichi 464-8601, JAPAN

The current status of Vlasov codes and future prospects of their application to space weather modeling researchare discussed. Due to their low noise level, Vlasov codes are widely used for studies of nonlinear wave-particleinteractions in plasmas. Vlasov code simulations are one of candidates for a future space weather modeling offull-kinetic processes in Geospace, because Vlasov codes are free from thermal fluctuations which is a greatadvantage over noisy particle-in-cell codes. On the other hand, we need a huge number of grid points in bothconfiguration and velocity spaces to suppress numerical diffusion, which is a disadvantage of current Vlasovcodes. In recent days, however, numerical interpolation schemes for Vlasov codes are rapidly developing. It isimportant to know the current Vlasov simulation techniques for a future studies of full-kinetic processes inGeospace.

- 164 -

P3-021

Numerical Analysis of Electron Acoustic Dromions and Its Application forBoundary Layer WavesS. S. Ghosh1, Y. Omura2, A. Sen3, and G. S. Lakhina1

1. Indian Institute of Geomagnetism, New panvel(W), Navi Mumbai, 410218, India2. RISH, Kyoto University, Uji, 611-0011, Japan3. Institute for Plasma Research, Bhat, Gandhinagar, 382428, India

With the advent of new technologies, high resolution, space-borne instruments are being utilized for in-depthstudy of the different regions of the magnetosphere, including the boundary layers. These observations arerevealing interesting insights of the previously known phenomena. One such observation is the existence of twodimensional structures in the Polar Cap Boundary Layer (PCBL) [1]. Modeling such multi-dimensional structuresis a contemporary challenge to space plasma physicists. In the previous studies, it has been shown that ananalytical solution of electron acoustic dromion may have a possible application to such observations [2,3]. In thepresent work, the analysis has been revisited by using a numerical algorithm whose parameter inputs are chosen tobe consistent with the satellite observation. It has been shown that, under appropriate boundary conditions, thedromion moves stably along the track determined by the boundaries. The collision of two dromions may resultfusion / fission of the two structures which, unlike the familiar soliton solution, may not preserve the number orshape of the structures. It has also been shown that an initial arbitrarily localized structure may evolve into adromion-like solution provided an appropriate time dependent boundary condition is maintained. Furthergeneralization of the algorithm may open the scope of its application to multidimensional structures observed inthe space.

References :[1] B. T. Tsurutani, C. M. Ho, G. S. Lakhina, B. Buti, J. K. Arballo, J. S. Picket and D. A. Gurnett,, Geophys.Res. Lett., vol. 25, pp. 4117 (1998).[2] S. S. Ghosh, A. Sen and G. S. Lakhina, Nonlinear Processes in Geophysics, vol. 9, pp. 463 (2002).[3] S. S. Ghosh, A. Sen and G. S. Lakhina, IEEE TPS,, vol. 32, pp. 1367 (2004).

- 165 -

P3-023

Results of Azerbaijani and Collaborative Regional Studies on SpaceWeather Potential Influence on Human Health and Physiological StateElchin S. Babayev1, F.R.Mustafa1, V.N.Obridko2, O.V.Khabarova3, I.Stoilova4, S. Dmitrova4, A.B.Asgarov1, and P.N.Shustarev 1

1. Shamakhy Astrophysical Observatory (ShAO), Azerbaijan National Academy of Sciences, 10, Istiglaliyyat Street, Baku,AZ-1001, Azerbaijan2. IZMIRAN, Russian Academy of Sciences, Troitsk, 142190, Moscow region, Russian Federation3. Space Research Institute (IKI), Russian Academy of Sciences, 117997, 84/32 Profsoyuznaya Street, Moscow, RussianFederation4. Solar-Terrestrial Influences Laboratory (STIL), Bulgarian Academy of Sciences, BAS Block 3, Acad. G. Bonchev Street,1113 Sofia, Bulgaria

Results of Azerbaijani and collaborative regional studies of potential influence of space weather changes onhuman health and physiological state are described. Links between space weather variations and sudden cardiacdeath, acute myocardial infarction mortality and morbidity, cardiac health state parameters and conductivity ofbiologically active points of human body (on the base of daily experiments) as well as dynamics of trafficaccidents are studied. Special attention was paid to the study of impacts of violent solar events and geomagneticstorms of various strengths on biological systems in middle latitudes.

P3-024

Mexican Space Weather Monitoring Station ProjectGuadalupe Munoz2 and Bernardo Vargas1

1. Escuela Superior de Ingenieria Mecanica y Electrica Zacatenco, IPN, Mexico D.F., Mexico2. Instituto de Geofisica, UNAM, Ciudad Universitaria, Mexico D.F., Mexico.

The main objective of this project is to establish a monitoring station to obtain daily data of the solar magneticactivity, as well as the main local weather parameter, to be able to develop space weather forecast and to studySun-Earth relations. The principal instruments to be developed are a coronagraph, with spectroscopic capabilitiesaimed to register the inner solar corona activity in the emission of Fe XIV line at 530 nm and a heliostat,observing mainly in the optical range and H-alpha. Some other instruments are needed in order to obtainimportant parameters on the Earth, like a piroheliometer, and meteorological instruments. The station will beplaced on the top of Cerro de las Animas, at 3070 meter high in Chapa de Mota, Estado de Mexico, around 100km from Mexico City.

- 166 -

P3-025

A Real-Time Magnetospheric Magnetic Field MonitorNatalia Yu. Ganushkina1, Marina V. Kubyshkina2, and Tuija I. Pulkkinen1

1. Finnish Metorological Institute, Space Research, POBox 503, FI-00101, Helsinki, Finland2. Institute of Physics, University of St.Petersburg, Petrodvoretz, Ulyanovskaya,1, 198504, Russia

One of the key elements of space weather studies is understanding of energetic particle (in particular, relativisticelectron) transport and energization processes. Because the energetic particle transport is strongly coupled to theelectromagnetic field variations, it is crucially important to have realistic models to electromagnetic fields.Accurate representation of the inner magnetosphere magnetic field is in great demand, but still missing. A uniquetool to provide a realistic representation of the magnetospheric magnetic field during geomagnetic storms hasbeen developed and is suitable for post-analysis of specific events. The model is based on an empiricalparametrization of magnetospheric current systems and use of in-situ magnetospheric measurements to define theintensity and location of these current systems for each time and location. This model can provide a nowcast forthe temporal evolution of the magnetic field in the inner magnetosphere. Furthermore, the model will be used toprovide short-time predictions of the Dst index, which is an important element of space weather warning systems.A real-time monitor of the magnetic conditions allows forecasters to assess risks and hazards to space-borne andground-based assets, while the continuous model output stream will provide a large database under a wide varietyof magnetospheric activity conditions for studies of the transport and acceleration processes.

P3-026

Relation of the Cross Polar Cap Potential to the Interplanetary ElectricFieldKeiichiro Fukazawa1, Tomoharu Aoyama, and Tatsuki Ogino

1. National Institute of Information and Communications Technology, Japan2. Solar-Terrestrial Environment Laboratory, Nagoya University, Japan

It is known that the cross polar cap potential is saturated under the strong interplanetary electric field. Varioussimulations have been done to clear the mechanism of that saturation and there are several ideas of the saturationeffect, however the accurate answer is not appeared yet. In this study, to investigate the influence of themagnetospheric dynamics to the cross polar cap potential, we conducted the global magnetohydrodynamicssimulation without the feedback effects from the ionosphere to the magnetosphere. The simulation ran withchanging the interplanetary magnetic filed (IMF) and the velocity of the solar wind to vary the interplanetaryelectric field. As the results of the simulation, the cross polar cap potential saturation only occurred at theincreasing the magnitude of southward IMF, not occurred at the increasing the velocity of the solar wind. Inaddition, the electric field of the dayside reconnection was saturated only for changing IMF and to see thecharacteristic configuration of the magnetic field line, reconnection rate decreased when the magnitude of IMFwas high. From these results, it is suggest that the saturation is caused by the decrease of reconnection rate due tothe shortage of carrying away the reconnected magnetic field line by the solar wind at the dayside under the strongsouthward IMF condition.

- 167 -

P3-027

Development of a MHD Code Satisfying Solenoidal Magnetic FieldCondition and Its ApplicationM.Yagi, K.Seki, and Y.Matsumoto

Solar-Terrestrial Environment Laboratory, Nagoya University, Furocho, Chikusa-ku, Nagoya, Aichi 464-8601, JAPAN

From the past observations by Mariner 10, it was suggested that the Mercury's magnetosphere might be analogousto the geomagnetosphere. The temporal and spatial scales of the Mercury's magnetosphere is, however, muchsmaller than those in the geomagnetosphere because of its week intrinsic magnetic field and dynamic pressure ofthe solar wind. It is pointed out that the kinetic effect, neglected in magnetohydrodynamics (MHD), may not benegligible in some regions of the Mercury's magnetosphere because of its small spatial scale compared withgyro-radius of ions. Statistical trajectory tracings of test particles (test particle simulation) is one of the important schemes toinvestigate the kinetic effect of particles. Recent studies by Delcourt et al. [2003; 2005] used analytical models ofelectric and magnetic fields that are obtained by rescaling the geomagnetosphere. And it is noted that resultantproperties largely depend on the field models. Thus usage of more realistic global field configuration of theMercury's magnetosphere might change some of results of the test particle simulations.In this study, we developed a new MHD simulation code that automatically satisfies solenoidal condition for themagnetic field (B) i.e., divB=0 to establish a self-consistent electric and magnetic field configuration of Mercury'smagnetosphere. It is noted that finite divB causes artificial acceleration/deceleration and satisfaction of thesolenoidal B field condition is important especially in the test particle simulations. To fulfill the condition, weused vector potential (A) instead of magnetic field itself in the MHD equation. The usage of the vector potentialautomatically guarantees div(rotA)=divB=0. For accurate simulation of high Reynolds number magnetofluid (lownumerical viscosity), we adopted R-CIP algorithm [Yabe et al., 1991; Xiao et al., 1996] to solve the advectionterm in the simulation code. The non-advection terms are solved by 3rd order Adams-Moulton predictor-correctormethod and 4th order Runge-Kutta method. The code assessment shows good ability of the developed MHD codein Alfven wave propagation, shock tube problem, and Kelvin-Helmholtz instability. A remarkable feature of thenew code with A is the precise description of Alfven wave propagation compared to the code with B even for highwave number regime near the Nyquist wavelength.After the code assessment, we apply this code to the global simulation of Mercury's magnetosphere. We devisedboundary conditions suitable for the vector potential code and solved perturbed magnetic field separately from thebackground magnetic field consisting of the mirror dipoles. The initial result with the constant solar wind showsformation of the bow shock, magnetopause, and cusp like structure at expected positions from the past study, andejection of plasmoid in the nightside magnetosphere. Now we are forming several models of inner boundary condition of planetary surface. In fact, it is not clear howto give the planetary surface because of its lack of observation. In the presentation, we will show detailedanalysis of resultant MHD fields in different boundary condition and its application to the statistical trajectorytracings of test particles.

- 168 -

P3-028

Magnetosphere-Ionosphere Coupling by the Global Hall-MHD SimulationJuntaro Kondo1, Tatsuki Ogino1, and Akira Kageyama2

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Japan2. JAMSTEC,3173-25, Showa-machi, Kanazawa-ku, Yokohama-city, Kanagawa, Japan

In the global MHD model, the ionosphere has been treated as a sheet model with electrical conductivity. However,the sheet model is not sufficient to essentially understand the magnetosphere-ionosphere coupling system. Weneed the 3D model to self-consistently solve structure and dynamics of ionosphere. When we calculatemagnetosphere-ionosphere coupling system in spherical geometry, it needs too long computation time.In this study, we adopt Yin-Yang grid composed of two identical spherical grids. The Yin-Yang grid wasdeveloped by Kageyama and Sato [2004]. By using this new grid, some problems that occur in high latituderegion of latitude-longitude grid are resolved. In addition Yin-Yang grid has some strong advantage that thecalculation is speedy, we can heighten accuracy easily, and it is also suitable for massively parallel computers.We have solved 3D Hall-MHD equations extended by adding Hall term and ion-neutral collision term for altitudesof 80-480 km where a small grid size of 1 km is used in the altitude direction. A static equilibrium solution ofionosphere is given at the initial state. The simulation result shows that the convection was given at an altitude of480 km as the upper boundary conditions to propagate toward the earth, and the current closure is formed in theionosphere.

P3-029

Nonlocal Memory Effects of the Electromotive Force on the Geodynamo orSolar DynamoKumiko Hori and Shigeo Yoshida

Graduate School of Environmental Studies, Nagoya University, Japan

The understanding of the solar dynamo mechanism is important for space weather. In the dynamo theory, 'the alpha-effect' is the key concept which connects the small-scale magnetic field with thelarge-scale field (e.g. Parker,1955). The alpha-effect represents the electromotive force, approximated to beinstantaneous in time and local in space. However, the approximation is valid only when Rm is smaller than 1,and inappropriate when the magnetic Reynolds number Rm is as large as that in the earth's core or the solarconvection zone. We introduce a function phi_{qr} as a nonlocal and non-instantaneous extension of the usual alpha-effect, andexamine its behaviour as a function of Rm for a kinematic dynamo model. We use G.O.Roberts(1972) flow,which has a non-zero helicity and two-dimensional periodicity. As a result, we find that the electromotive force for Rm > O(1) has a nonlocal memory effect, which stronglyaffects the dynamo action, while we confirm that the electromotive force when Rm is smaller than 1 can beapproximated by the local alpha-effect. The results demonstrate that the nonlocal memory effect of theelectromotive force is important in the geodynamo or the solar dynamo.

- 169 -

P3-030

Particle and Field Characteristics of Broadband Electrons Observed byFAST during Geomagnetic Storms: A Multievent StudyAkimitsu Nakajima1, Kazuo Shiokawa1, Kanako Seki1, James P. McFadden2, Charles W. Carlson2, Robert J. Strangeway3, and Kiyofumi Yumoto4

1. Solar-Terrestrial Environment Laboratory, Nagoya University, Chikusa-ku, Nagoya 464-8601, Japan2. Space Sciences Laboratory, University of California Berkeley, Berkeley, CA 94720-7450, USA3. Institute of Geophysics and Planetary Physics, University of California Los Angeles, Los Angeles, CA 90024-1567, USA4. Space Environment Research Center, Kyushu University, Higashi-ku, Fukuoka 812-8581, Japan

During geomagnetic storms, remarkable flux enhancements (> 10^13 eV cm^-2 s^-1) of precipitating electronsover a broad energy range (~0.05-30 keV) are sometimes observed near the equatorward edge of the auroral oval.The electron flux enhancements are called broadband electrons (BBEs). We identified twelve BBE events fromelectron energy spectra obtained by the FAST satellite during 81 large geomagnetic storms (minimum Dst index <-100 nT) between September 1996 and March 2004. Ground-based magnetic field data show that the BBEs tendto occur ~6-28 min after the onset of substorm during the main phase of geomagnetic storms. During these events,pitch angle distribution of the electrons is isotropic at a higher energy range above ~1 keV except for a loss-conefeature around the field-aligned upward direction. At a lower energy range below ~1 keV, field-aligned downwardelectron fluxes are most intense and the perpendicular fluxes are weakest. These results imply that a higher energypart of the BBEs originated from higher altitudes in the inner magnetosphere and that a lower energy part wasaccelerated parallel to the local magnetic field at lower altitudes near the satellite. Intense fluctuations of electricand magnetic fields and enhanced low-frequency (0.1 Hz-16 kHz) waves are observed during the all BBE events.We compare low-energy (below 1 keV) electron fluxes and wave Poynting fluxes. For most BBE events, thecalculated Poynting flux is systematically downward with comparable intensity to that of low-energy electronfluxes, suggesting downward acceleration of low-energy electrons by the observed low-frequency waves.

P3-031

Parametric Decay of Circularly Polarized Alfven Waves in the RadiallyExpanding Solar WindShin Tanaka, Tatsuki Ogino, and Takayuki Umeda

Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan

We present an MHD simulation study of the parametric decay of the circularly polarized Alfven wavespropagating in the radial outflow of the solar wind. Assuming the transonic wind solution as an initial condition,we continuously injected monochromatic circularly polarized Alfven waves from the inner boundary at the lowercorona, and simulated the wave propagation. The injected Alfven waves are subject to the parametric decay, anddensity fluctuations in the solar wind plasma grow rapidly at a specific region. The location of the most unstableregion depends on the amplitude and frequency of injected Alfven waves. We found that the unstable region ofsimulation results can be well estimated by considering a localized dispersion relation in the frame of referencemoving with the background solar wind.

- 170 -

P3-032

Cluster Observations of Electrostatic Solitary Waves near theQuasi-perpendicular ShockY. Hobara1, M. A. Balikhin1, S. N. Walker1, M. Andre2, and M. Dunlop3

1. Department of Automatic Control & Systems Engineering, University of Sheffield, Sheffield, UK2. Swedish Institute of Space Physics, Uppsala, Sweden3. Space Sciences Division, Rutherford-Appleton Laboratory, UK

We analyzed a number of electrostatic solitary waves (ESWs) observed in the foot region of Earth'squasi-perpendicular bow shock by Cluster. By utilising the four probe potential measurements sampled at 9kHzby the Cluster Electric Field and Wave (EFW) instrument it is possible to calculate two sets of parallel electricfield components. These measurements are then used to investigate the fundamental wave properties such as thewave normal vector, propagation speed and potential structure. ESWs with a bipolar electric field signatureexhibit negative potentials indicative of ion depletion structures (e.g. Ion hole). Isolated monopolar and tripolarelectric field signals are also observed implying a finite potential drop across the structure (e.g. weak doublelayer). The experimentally derived wave properties are compared with similar observations in different regions ofthe magnetosphere and also theoretical predictions. These properties are then used to identify the possible wavemode and generation mechanisms.

P3-033

Energy Input Estimated by NOAA- Satellites during Magnetically Quiet andStorm Conditions at Geo-space Environment during a Solar MinimumPeriod.Raman Selvamurugan, B M Pathan, Ajay Dhar , and Arun Hanchinal

Indian Institute of Geomagnetism, plt#5, Sec-18, Kalamboli Highway, New Panvel, Navi Mumbai 410 218

The total energy detector average energy input estimated by the NOAA-satellite to the southern latitudes betweenthe equator to pole during quiet and disturbed time reveal that the energy input can be higher by about 5-6 timesfor intense cases of disturbances (Dst>-70 nT). The increase in energy seems to vary considerably for variousevents occurred at various occasions of a solar minimum year for latitudes beyond 50º at both southern andnorthern hemispheres. The energy associated with the increased solar wind particles found to have correlationswith the occurrences of Coronal mass emissions (CME) those have resulted in effecting geo-magnetic storm andsubstorms. The total energy detector average energies recorded by NOAA satellites explain that the latitudinalenergy input for both the hemispheres remained unequal and the southern hemispherical input remained higherthan the northern latitudes for most of the disturbance cases. The local time dependence of the energy inputs onquiet time reveal that there could be two sectors one in the early after noon hours and an another in the pre-noonhours during when there is a broad peak observed. However, such distinction in local time dependence duringdisturbance conditions seem to rather not exist and it is supposedly be depending on various factors such as thetransit time of CME, flares and shock arrivals etc., which cause storms and substorms in the geospaceenvironment.

- 171 -

P3-034

Relativistic Turning Acceleration of Radiation Belt Electrons byWhistler-mode ChorusYoshiharu Omura1, Naoki Furuya1, and Danny Summers2

1. Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Kyoto 611-0011, Japan2. Department of Mathematics and Statistics, Memorial University of Newfoundland, St. John's, Newfoundland, Canada

We perform test particle simulations assuming whistler-mode chorus wave packets that are generated at thegeomagnetic equator propagate away from the equator in both poleward directions. While electrons in the energyrange 10 - 100 keV are primarily responsible for the generation of chorus waves through pitch angle diffusion intothe loss cone, it has been found that a fraction of the higher-energy electrons from a few hundred keV to a fewMeV are effectively accelerated by chorus due to a special nonlinear trapping process called relativistic turningacceleration (RTA). The RTA process takes place for a wave packet with variable frequency such as thatoccurring in a rising tone of chorus emissions. We study the efficiency of the RTA process for different particleenergies. A Green's function method is used to describe the evolution of the particle energy distribution function. The RTA process due to chorus emissions creates a high-energy tail in the electron energy distribution function.The shape of the high-energy tail is determined by the distribution function of the seed electrons in thelower-energy range. RTA can accelerate electrons in a much shorter timescale than that estimated by quasi-lineardiffusion theory, e.g., it typically takes tens of minutes to hours for a few 100 keV seed electrons to be acceleratedto energies of a few MeV by RTA. RTA is a viable process for generating relativistic electrons in the Earth'sradiation belt.

P3-035

MHD Modeling for the Global Solar CoronaTakuma Matsumoto, Eiji Asano, and Kazunari Shibata

Kwasan and Hida observatory

We have developed three dimensional spherical magnetohydrodynamic simulation code by using CIP-MOCCTmethod in order to investigate the properties of the global solar corona and solar wind. Some test simulationsreveal the high performance of our algorithms. Next, we have implemented the simulations for the global coronaincluding the solar wind until the steady state is obtained. As the boundary condition, we use magnetic fieldobservation to make a simulation more realistic. Like other simulations, our results also show the qualitativeproperties of the solar wind structures. Finally, advanced treatment for the boundary conditions of the coronalbase are discussed. The idea of characteristics of hyperbolic equations makes the numerical solutions more stableand physically consistent. Numerical techniques discussed in this chapter will help us incorporate observationaldata in the coronal models and improve them significantly. We believe that our simulations will be a quiteefficient tool for the space weather researches.

- 172 -

P3-036

IMF Sector Dependent Directional Anisotropy and Gradient of GalacticCosmic Ray Measured by the Muon Detector NetworkYoshitaka Okazaki1, Kazuoki Munakata2, Akira Fushishita2, and Takuya Narumi 2

1. Department of Geophysics, Tohoku University, Japan2. Faculty of Science, Shinshu University, Japan3. School of General Education, Shinshu University, Japan4. Bartol Research Institute, University of Delaware, USA5. Australian Government Antarctic Division, Australia

Interplanetary magnetic field (IMF) sector (away and toward) dependent directional anisotropies of galacticcosmic ray (GCR) are investigated by using the data obtained from the Muon detector network. The results of thisstudy are summarized as follows. (1) Northward (southward) directional anisotropy is measured when the IMF isdirected toward (away from) the Sun. We also investigate This relationship qualitatively shows an agreement withthe GG index proposed by the Mori and Nagashima [1979]. (2) It is found that the north-south directionalanisotropy in the GSE coordinate has seasonal variations. One possible reason would be tan orientation of the IMFin the GSE coordinate (geometrical effect). We will discuss the cause for this. (3) Sector dependent fractionaldensity gradient indicates that GCR density has its local maximum (minimum) at the heliospheric current sheetwhen the solar magnetic polarity is positive (negative). This result supports the latitudinal density distributioncalculated by the model [Kota and Jokipii, 1983]. We will report these results.

P3-037

Statistical Analysis of Spectral Parameters of Pc5/Pi3 GeomagneticFluctuations Inside and Outside the Magnetosphere: Noise or Non-linearity?Nadejda V. Yagova1, Vyacheslav A. Pilipenko1, Dmitry Yu. Klimushkin2, and Mark Engebretson3

1. Institute of the Physics of the Earth, Moscow2. Institute of the Solar-Terrestrial Physics, Irkutsk3. Augsburg College, Augsburg, USA

We analyze the parameters of the geomagnetic noise in the frequency range 1-4 mHz (Pc5/Pi3) from WINDsatellite in the interplanetary space and more than 50 observatories from polar to middle latitudes and in a widerange of MLT. The analysis is performed in the following way: 1) spectral parameters are estimated in 2-hour running window at each station; 2) signal is decomposed into an elliptically polarized (P) and randomly polarized noisy (N) components; 3) for each component the spectrum is presented in a log-log scale and expanded over Legendre polynomials.The spectral parameters, their diurnal variations and dependence on the space weather parameters turned out to benot identical for P and N components. Pi3 spectral amplitude varies in a correlated way in the interplanetary space and on the ground from polar tomiddle latitudes in all MLT sectors. Essentially positive correlation between stations also exists for higher spectralmoments (spectral slope and the parameters describing the spectral form) on the ground, but we have not foundany external parameter responsible for this correlation. We assume that the positive correlation on regional scalefor higher spectral moments is caused by intra-magnetospheric mechanisms. The important feature of the ULFactivity inside the magnetosphere is a statistically significant correlations between their amplitude and higherspectral moments, whereas a similar correlation is absent in the extra-megnetospheric ULF activity. Thisdependence is more evident in the N-component, showing that the so-called ULF noise is partly the result of amagnetospheric non-linearity.

- 173 -

P3-038

Development Plan of Electric Field and Plasma Wave Investigations forFuture Space Weather MissionsY. Kasaba1, A. Kumamoto1, T. Ono1, M. Iijima1, H. Kojima2, Y. Ueda2, Y. Omura2, S. Yagitani3, Y. Kasahara3, Y. Goto3, T. Imachi3, K. Ishisaka4, T. Okada4, A. Matsuoka5, and Electric Field and Plasma Wave Investigation Team

1. Tohoku Univ.2. Kyoto Univ.3. Kanazawa Univ.4. Toyama Pref. Univ.5. JAXA

The space weather mission, electric field and plasma wave investigation is important for the clarification globalplasma dynamics and energetic processes in the space weather studies. We have several missions which willcontribute those objectives:The small-sized radiation belt mission, ERG (Energization and Radiation in Geospace), and the cross-scaleformation flight mission SCOPE/XScsale. Those will prevail the universal plasma mechanism and processes inthe Geospace laboratory. Those missions are also coupled with planetary plasma studies planned in ourcommunity, i.e., the BepiColombo mission to Mercury, small-sized space telescope TOPS, and the small-sizedand full-scale Jovian mission in future.The main purposes of electric field and plasma wave observation for those missions are: (1) Examination of thetheories of high-energy particle acceleration by plasma waves, (2) identification of the origin of electric fields inthe magnetosphere associated with cross-scale coupling processes, (3) diagnosis of plasma density, temperatureand composition, and (4) investigation of wave-particle interaction and mode conversion processes. Simultaneousobservation of plasma waves and energetic particles with high resolution will enable us to investigate thewave-particle interaction based on quasi-linear theory and non-linear models. In order to achieve those objectives, the instrument including sensitive sensors (the long wire / stem antennae, thesearch-coil / loop antennae) and integrated receiver systems are now in development. Direct identification ofnonlinear wave-particle interactionsassociated will be tried by waveparticle correlator. In this paper, we will summarize the current plan & efforts forthose future activities.

- 174 -

P3-039

DP2 Fluctuations of the Ionospheric Electric Field Observed by FM-CW HFRadarManabu Shinohara1, Akihiro Ikeda2, Kenro Nozaki3, Vasily V. Bychkov4, Boris M. Shevtsov4, and Kiyohumi Yumoto1

1. Space Environment Research Center, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka2. Department of Earth and Planetary Sciences, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka3. National Institute of Information and Communication Technology, 4-2-1 Nukuikitamachi, Koganei, Tokyo, Japan4. Institute of Cosmophysical Research and Radiowaves Propagation (IKIR) of the Far Eastern Branch of Russian Academy ofSciences

DP2 type geomagnetic fluctuations are characterized by quasi-periodic variations with time scales of about 30minutes to several hours. Southward turnings of the interplanetary magnetic field are main cause of DP2fluctuations. The equivalent current system of DP2 fluctuations consists of two vortices in the polar region. Andthe ionospheric electric field penetrates to the low latitudes and the equatorial region.In the dayside dip equator, the ionospheric current is strongly amplified by the localized conductivityenhancement (Cowling effect). Accordingly, magnetic fluctuations are amplified. By using this peculiarity, thezonal electric field in the ionosphere can be estimated from the magnetic field measurement. On the other hand,the ionospheric conductivity decreases in nighttime. Therefore, electric field fluctuations in the ionosphere cannotbe observed from magnetic variations. In order to observe ionospheric electric field fluctuations in nighttime, thedirect observation of the ionosphere by the HF radar is needed.By using the FM-CW (Frequency Modulated Continuous Wave) HF radar network of the low latitude station atSasaguri, Japan and the mid latitude station at Paratunka, Kamchatka, Russia, DP2 type fluctuations ofionospheric electric field were observed. DP2 fluctuations observed by the HF radar in nighttime correlated withDP2 magnetic fluctuations observed in the polar region and the dayside dip equator. The dawn to dusk electricfield was found at both the dayside equator and the nightside low latitudes. The latitudinal dependence of theelectric field amplitude observed at the mid and low latitude stations is discussed.

P3-040

Observational Consequences of Reconnection in the Solar Corona and theMagnetosphereK. Reeves, W. J. Hughes, K. Korreck, J. Lin, J. Raymond, N. Schwadron, H. Spence, and D. Webb

Harvard-Smithsonian Center for Astrophysics, USA

Reconnection occurs in both the solar corona and the magnetosphere. Although these two environments aredifferent in many ways, the manifestations of reconnection are remarkably similar. For example, the X-RayTelescope (XRT) on Hinode has observed the effects of magnetic reconnection in solar flares, including field lineshrinkage (or dipolarization) and supra-arcade downflows. Similarly, dipolarization and bursty bulk flows areobserved because of reconnection in the magnetotail. The similarities and differences of these phenomena in themagnetosphere and solar corona will be presented. Thus, we explore observational evidence for reconnection as auniversal plasma process.

- 175 -

P3-041

Characteristics of Fine-Scale Auroras Obtained from Simultaneous Reimeiand Ground-based ObservationsTakeshi Sakanoi1, Kazushi Asamura2, Masafumi Hirahara3, Yasuyuki Obuchi1, Harald U. Frey4, Masaki Okada5, Yusuke Ebihara6, Kanako Seki6, Yasumasa Kasaba1, Eric Donovan7, Steven B. Mende4, and Brian Jackel7

1. Tohoku University, Sendai, 980-8578, Japan2. JAXA/ISAS, Sagamihara, 229-8510, Japan3. Rikkyo University, Ikebukuro, 171-8501, Japan4. U. C. Berkley, Berkeley, CA, 94720-7450, USA5. NIPR, Itabashi, 173-8515, Japan6. STEL, Nagoya University, Nagoya, 464-8601, Japan7. U. Calgary, 2500 University Drive, Calgary, Alberta, T2N 1N4, Canada

To clarify fine-scale auroral dynamics, we examined the fine-scale characteristics of discrete, pulsating aurora andblack aurora using simultaneous image and particle observation data by a multi-spectral aurora camera (MAC)and particle sensors (ESA and ISA) on board the Reimei satellite at an altitude of 640 km. Three emissions of N2+1N (427.8 nm), OI (557.7 nm) and N2 1P (670 nm) are independently obtained by the MAC with typical spatialand time resolutions of 1 km and 120 ms, respectively. Energy range and time (spatial) resolution of particlesensors are 10 eV/q - 12 keV/q, 40 ms (300 m), respectively. In addition, coordinated Reimei and ground-basedobservations have been carried out in northern and southern hemispheres using data obtained at THEMISground-based observatories (GBOs) and Syowa station, Antarctica, respectively. On the spatial structures morethan 2 km, it is found that there is one-to-one correspondence between auroral emission and precipitatingelectrons. We have also clarified the characteristics of precipitating electrons corresponding to fine-scale auroralshear motions, pulsating and black auroras. In this talk, recent results of fine-scale auroral structures obtainedfrom Reimei and simultaneous ground-based observations will be presented in detail.

P3-042

Turbulent Natures of the Kelvin-Helmholtz Instability and Its Application tothe Sun-Earth Connection ModelYosuke Matsumoto1 and Kanako Seki2

1. Graduate School of Environmental Studies, Nagoya University2. Solar-Terrestrial Environment Laboratory, Nagoya University

The entry process of the solar wind plasma into the magnetosphere during the northward IMF condition has beencontroversial in contrast to the Dungey's reconnection model for the southward IMF case. The major candidateprocesses are the double lobe reconnection model [Song et al., 1999], in which newly closed magnetic field lineson the dayside magnetopause capture the solar wind plasma, and the turbulent transport by the Kelvin-Helmholtzinstability (KHI) driven by the fast solar wind flow. We have shown by simulation studies that the strong flowturbulence is a natural consequence of the nonlinear development of the Kelvin-Helmholtz instability (KHI)through the secondary instability [Matsumoto and Hoshino, 2004, 2006]. More recently, we studied the 3-Dnonlinear evolution of the KHI by performing MHD simulations [Matsumoto and Seki, 2007]. The KH vortex isalso susceptible to "the 3-D secondary instability" which converts the rotating energy into the magnetic energy bygenerating large amplitude magnetic fluctuations. We found that the nonlinear evolution of such large amplitudemagnetic fluctuations is subject to turbulence: Once the 3-D secondary instability is excited, the mode cascadestarts after the amplitude of the fluctuation reaches a certain level with respect to the background field. Thepresent result implies that even in a strong magnetic field condition, generation of turbulence can be achieved bythe 3-D secondary instability. The detailed mechanism of the turbulent natures of the KHI and its application tosolar wind-magnetosphere interactions are discussed in this presentation.

- 176 -

P3-043

Data Assimilation for Modeling the Ring Current EvolutionShin'ya Nakano2, Genta Ueno1, Yusuke Ebihara3, Mei-Ching Fok4, Shin-ichi Ohtani5, Pontus C:son Brandt5, Donald G. Mitchell5, Kunihiro Keika6, and Tomoyuki Higuchi1

1. The Institute of Statistical Mathematics, ROIS, Minato City, Tokyo 106-8569, JAPAN2. Japan Science and Technology Agency, Chiyoda City, Tokyo 100-0004, JAPAN3. Institute for Advanced Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, JAPAN4. NASA Goddard Space Flight Center, Code 612.2, Greenbelt, MD 20771, USA5. The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723-6099, USA6. Oesterreichische Akademie der Wissenschaften, Institut fuer Weltraumforschung, Schmiedlstrasse 6, 8042 Graz, Austria

In order to obtain a realistic model of the ring current evolution, we assimilated ENA data from the IMAGEsatellite into a kinetic ring current model (CRCM) by Fok et al. (2001) using an algorithm based on the particlefilter/smoother. It was assumed that the electric potential distribution, plasmasheet ion density, and plasmasheetion temperature were uncertain, and they were estimated through the data assimilation process. On the basis of theestimates of those parameters, the ring current ion distribution in the inner-magnetosphere was consequentlyestimated. In this study, this data assimilation technique was applied to some magnetic storm events. We discussthe relationship between the electric potential structure and the ring current distribution for the storm.

P3-044

MAGDAS Preliminary ResultsKiyohumi Yumoto1, Teiji Uozumi1, Yuki Hirayama2, Akihiro Ikeda2, and MAGDAS Group

1. Space Environment Research Center, Kyushu University 6-10-1 Hakozaki, Higashi-ku, Fukuoka2. Graduate School of Science, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, JAPAN

The Space Environment Research Center (SERC), Kyushu University is installing the MAGnetic Data AcqusitionSystem (MAGDAS) at 50 stations in the Circum-pan Pacific Magnetometer Network (CPMN) region, and severalFM-CW radars along the 210 magnetic meridian. The MAGDAS project has the potential to contribute greatly toIHY/CAWSES by supporting ground-based magnetometer array for worldwide studies, and by demonstrating thebeauty, importance, and relevance of space science to the world. Nearly 20 and 10 MAGDAS units were installedin collaborations with 30 organizations in the world, respectively, along the 210 magnetic meridian in 2005 andalong the magnetic dip equator in 2006. In the year 2007, 20 MAGDAS units will be deployed in places such asSouth Africa, India, Italy, Mexico, Alaska, Siberia, and Antarctica. The goal of MAGDAS is to become the mostcomprehensive ground-based monitoring system of the earth's magnetic field.In the present paper, we will introduce preliminary results obtained from MAGDAS Project; (1) We comparedlong-term spectrum peaks of solar wind parameters, geomagnetic indices, and MAGDAS data to understandcouplings of the solar wind- magnetosphere-ionosphere-atmosphere system. The spectrum peaks of 7.5, and 14.5day period on the equatorial MAGDAS data mean a strong interaction of the atmospheric neutral wind and theionospheric Sq current. (2) Pi 2 pulsations at the world-widely separated stations near the dip equator are found toshow an amplitude enhancement around each 10:00-13:00 local time. The closer the observation site is to themagnetic dip equator, the amplitudes tend to become larger. (3) From analysis of SC-associated electric fieldsobserved by FM-CW radar at Sasaguri, we found a superimposed effect of the polar electric field and thewestward electric field of compressional hydromagnetic wave, which were caused simultaneously by theinterplanetary shocks.

- 177 -

P3-046

Characteristics of Equatorial Pi 2 Pulsations Observed at the MAGDASStationsYuki Hirayama1, Kiyohumi Yumoto2, Teiji Uozumi2, Terumasa Tokunaga1, Shinichi Watari3, and MAGDAS/CPMN Group

1. Graduate School of Science, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, JAPAN2. Space environment Research Center, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, JAPAN3. National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795,JAPAN

At the onset of magnetospheric substorms, impulsive hydromagnetic oscillations with periods of 40-150 sec, socalled Pi 2 magnetic pulsations, occur globally in the magnetosphere. In order to investigate characteristics of the equatorial Pi 2 pulsations, we analyzed magnetic data obtained fromMAGDAS stations AAB, LKW, CEB, DAV, ANC, EUS and YAP, which were located near the dip equator.Time resolution of the magnetic data is 1 sec. Magnetic data were bandpass-filtered (40 to 150 sec) beforeselecting Pi 2 events . About 200 Pi 2 events were selected for the period of January 1-31, 2007.We investigate the local-time dependence of the H-component wave amplitude of equatorial Pi 2 pulsations.These amplitudes were averaged in each hour bin. It is found that the amplitude enhancement of Pi 2 pulsationsoccurred within each interval of 8-16 local-time at near the dip equatorial stations.Furthermore, we analyzed magnetic data observed at CEB, DAV and YAP in order to investigate latitudinaldependence of Pi 2 amplitude in the equatorial region. These stations provided the advantage to examine therelationship between Pi 2 amplitude and the Dip Lat., because these stations were located in almost the same localtime, and in almost the same ambient total field intensity. We can conclude that as closer the observation site waslocated near the dip equator, the Pi 2 amplitudes tended to become larger.

P3-047

A New Index to Monitor Temporal and Long-Term Variations of theEquatorial Electrojet by MAGDAS/CPMN Real-Time Data: EE-IndexTamiki Ueno1, Kiyohumi Yumoto2, Teiji Uozumi2, Kentaro Kitamura3, Shuji Abe2, Yuji Numata1, and MAGDAS group2

1. Graduate School of Sciences, Kyushu University, 6-10-1, Hakozaki, Higashi-ku, Fukuoka 812-8581,Japan.2. Space Environment Research Center, Kyushu University, 6-10-1, Hakozaki, Higashi-ku, Fukuoka 812-8581,Japan.3. Department of Mechanical & Electrical Engineering, Tokuyama College of Technology, 3538 Takajo, Kume, Shunan,Yamaguchi 745-8585 JAPAN.

A new index; EE-index (EDst, EU, and EL) is proposed to monitor temporal and long-term variations of theequatorial electrojet (EEJ) by using the MAGDAS/CPMN real-time data. The mean value of the H componentmagnetic variations observed at the nighttime (LT = 18-06) MAGDAS/CPMN stations along the magneticequatorial region is found to show variations similar to those of Dst; we defined this quantity as EDst. The EDstcan be used as a proxy of Dst for the real-time and long-term geospace monitoring. By subtracting EDst from theH component data of each equatorial station, it is possible to extract the Equatorial Electrojet and CounterElectrojet components, which are defined as EU and EL, respectively.We investigated the occurrence characteristics of the EEJ (EU) component derived from Davao (DAV) station(GMLAT=-1.37deg, GMLON=196.53deg). We analyzed EU data for the period from July 1, 2005 to March 4,2006. During the period, several magnetic storm activities occurred and sometime EEJs were strongly disturbed.In those cases, it is not clear to identify the occurrence of EEJ from the raw magnetogram. Nevertheless, EU madepossible to identify the disturbed-time EEJ component similar to those of the quiet period. It is found that theamplitude of the extracted component fluctuated with dominant peak periods of 7.5, 14.5 and 35.3 day. The resultsuggests that the activity of the EEJ correlates with the Rossby wave. This issue should be clarified in the futurework.

- 178 -

P3-048

Correlations between the Variations of the Radiation Belt Electron Fluxesand Pc5/Pi3 Parameters at Timescales About Several DaysVyacheslav A. Pilipenko1, Nadejda V. Yagova1, and Dmitry Yu. Klimushkin2

1. Institute of the Physics of the Earth, Moscow2. Institute of the Solar-Terrestrial Physics, Irkutsk

The correlations of the radiation belt electron fluxes Je with the ULF (1-4 mHz, the frequency range of Pc5/Pi3geomagnetic pulsations) spectral power S and other spectral and polarization parameters are analyzed. Thesecorrelations have been examined at different timescales in dependence on electron energy, orbit and stationposition. Several years of electron observations at geostationary satellites LANL and highly elliptical satelliteCRRES, and geomagnetic fluctuations at more than 30 ground stations from middle to polar latitudes areanalyzed. The interdependent factors, influencing simultaneously both Je and ULF wave intensity, such as thesolar wind velocity, are discriminated to reveal a direct driver of Je enhancements. The diurnal and solar cycle27-day variations have been excluded. The Je - S correlations for short-time irregular variations become positiveat some time shift t. This shift is about zero for electrons with energies below 300 keV, and it grows with electronenergy and L-value, reaching 1.5-2 days for relativistic energies at L>5. Possible mechanisms of the observed Je -S relations are discussed.

P3-049

Plasma Sheet Contribution to the Ring Current during Storm-Time Isolatedand Periodic SubstormsFiori-Anastasia Metallinou1, Ioannis A. Daglis1, Thomas E. Moore2, Mei-Ching Fok2, and Dominique C. Delcourt3

1. National Observatory of Athens, Institute for Space Applications and Remote Sensing, GR-15236 Penteli, Greece2. Laboratory for Geospace, NASA Goddard SFC, Greenbelt, MD 20771 US??3. Centre d'etude des Environnements Terrestre et Planetaires, Centre National de la Recherche Scientifique, F-94107Saint-Maur des Fosses&

In this study we simulate storm-time substorms isolated and periodic ones by using a three-dimensional dynamicion-tracing model. We follow the transport and acceleration of ions, under the influence of a backgroundconvection electric field with a superposed impulsive electric field due to magnetic field dipolarizations, asobserved by spacecraft during substorm expansion. We examine the relative influence of O+ and H+ ionsoriginating in the plasma sheet on the ring current development. Maps of the temporal and spatial variations of ionenergy densities in the inner magnetosphere are constructed. Initial results suggest that the difference inenergization is much more prominent for O+ ions, which have been observed to be preferentially accelerated bysubstorm-induced electric fields. Multiple periodic substorms have a distinctly cumulative effect on the ringcurrent development, influencing both the earthward penetration and the energization of ions.

- 179 -

P3-050

Conjugate Ionospheric Perturbations during Magnetic Storms: Evidence forStormtime M-I CouplingJ. C. Foster, P. J. Erickson, and W. Rideout

MIT Haystack Observatory, Westford, MA 01886, USA

In the early phases of a geomagnetic storms, the low and mid-latitude ionosphere are greatly perturbed. Promptpenetration electric fields uplift and redistribute the low-latitude ionosphere plasma. In the plasmasphere boundarylayer, the sub-auroral polarization stream electric field (SAPS) forms as pressure gradients at the inner edge of themagnetospheric ring current drive Region-2 field-aligned currents into the evening-sector ionosphere. Largepoleward-directed electric fields at ionospheric heights are set up to drive closure currents across thelow-conductivity region equatorward of the auroral electron precipitation. These large SAPS electric fields mapup into the ring current and inner magnetosphere where the inward extent of the SAPS overlaps and erodes theouter plasmasphere and mid-latitude ionosphere, drawing out extended plumes of storm enhanced density (SED).The SED plumes can be used as a tracer of the location and strength of disturbance electric fields. Recentobservations indicate that many of these mid-latitude ionospheric disturbance features exhibit degrees of magneticconjugacy and simultaneity which implicate the workings of the electric fields which couple the high and lowaltitude regions. This presentation will emphasize the combined use of satellite and ground-based observations to investigate thedegree of magnetic conjugacy associated with specific features of the stormtime ionospheric perturbation. It isfound that features related to the workings of the SAPS electric field - associated with magnetospheric drivers inthe stormtime ring current - exhibit clear, striking conjugacy characteristics. TEC enhancements oninner-magnetospheric field lines exhibit localized and longitude-dependent features which are not strictlymagnetically conjugate.

P3-051

SIEVERT: A Space Weather Application to Account for Radiation aboardAircraftNicolas Fuller1, Pierre Lantos+1, J.F. Bottollier-Depois 2, and Francois Trompier2

1. Paris Observatory, LESIA, 92190 Meudon, FRANCE2. IRSN, B.P. 17, 92262 Fontenay-aux-Roses, FRANCE

Galactic cosmic radiations and Solar particles impacts the Earth giving increased radiation doses at aircraftaltitudes. The computerized system for flight assessment of exposure to cosmic radiation in air transport(SIEVERT) is delivered to airlines for assisting them in the application of the European directive concerningradiation doses, especially in France where this system was developped. This tool allows airline companies toassess doses for each aircrew member and also permits anyone to estimate the dose on a given flight via theSIEVERT web site (www.sievert-system.org). The system takes into account both solar and cosmic radiations,using the specific calculation of SiGLE semi-empirical model to estimate radiation doses in case of a GLE. Wepresent the principle of both SIEVERT and SiGLE and give a first assessment after seven years since it started.This project was developped by DGAC (French Directorate of Civil Aviation) and partners: IRSN (Institute forRadiation Protection and Nuclear Safety), Paris Observatory and IPEV (French Institute for Polar Research).(+ Pierre Lantos died on March 1st 2007)

- 180 -

P3-052

Density Gradients and EMIC Wave Source Location in thePlasmasphere-MagnetosphereFraser, Brian J1, Singer, Howard J2, Moldwin, Mark B3, Goldstein, Jerry4, and Thomsen, Michelle F5

1. Centre for Space Physics, University of Newcastle, Callaghan, NSW 2308, Australia2. NOAA/SEC, 325 Broadway, Boulder, CO 80305, USA3. Department of Earth and Space Sciences University of California, Los Angeles, CA 90095-1567, USA4. Space Science and Engineering Division, Southwest Research Institute, TX 78227, USA5. Space and Atmospheric Science Group, Los Alamos National Laboratory, Los Alamos, NM 87545, USA

Electromagnetic ion cyclotron (EMIC) waves play an important role in magnetosphere dynamics including ringcurrent ion and radiation belt electron losses. In order to quantify the role of the waves the distribution of EMICwave power and frequency with time throughout the magnetosphere is important. Also important is the role ofdensity gradients in the plasmasphere and magnetosphere in creating instability. It has generally been assumed inthe past that the steep density gradient in the radial density profile of the magnetospheric plasma, the plasmapause,is the favoured region for the generation and propagation of electromagnetic ion cyclotron (EMIC) waves. This isthe region of overlap between the expanding cold plasmasphere with the inner edge of the hot ring current duringstorm recovery, providing favourable conditions for EMIC instability. The plasmapause is also expected toprovide a convenient gradient for guiding waves from equatorial sources to higher latitudes. Although EMICwaves are seen at the plasmapause, they have been seen more frequently by AMPTE and CRRES outside theplasmapause. More recently extended radial plasma plumes, attached to the plasmasphere have been seen inIMAGE-EUV data. These provide enhanced radial plasma density and associated azimuthal gradients. UsingCRRES, GOES, LANL and IMAGE-EUV data the role of plasma gradients in determining EMIC source locationand propagation properties will be considered using case studies and statistics. These results will provide anindication of the conditions under which EMIC waves generation occurs in the magnetosphere.

P3-053

Nonlinear Force-Free Magnetic Field Extrapolation in Open Space above aSpherical Surface Based on the Direct Boundary Integral FormulationHan He and Huaning Wang

National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012,China

The direct boundary integral equation (DBIE) was proposed by Yan & Li (2005, 2006), which can be used toextrapolate the nonlinear force-free magnetic field in the solar atmosphere. The formulations of DBIE can beapplied to the infinite plane surface boundary geometry, as well as to the spherical boundary geometry. Based onthe DBIE, we try to construct a practical calculation scheme for the nonlinear force-free magnetic fieldextrapolation in open space above a spherical surface. The field is calculated layer by layer in our scheme. Wewill present preliminary results of the test calculations by using the analytical force-free solutions given by Low &Lou (1990).

- 181 -

P3-054

Multi-scale Three-Dimensional MHD Simulation for the Fast MagneticReconnectionAtsuhiko Kondo, Tohru Shimizu, and Masayuki Ugai

Department of computer science, Ehime university, Bunkyo town, Matsuyama city 790-8577

The fast magnetic reconnection is an important topic in explosive space plasma phenomenon but has difficultproblems to study numerically. Speaking in the limit of MHD model, the largest problem is that the magneticdiffusion region which is extremely narrow actively controls the whole of the reconnection region including theejected plasmoid far from the region. Hence, in the numerical MHD study, the magnetic diffusion region must beresolved with a high resolution and the whole of the reconnection region must be also resolved as a response forthe magnetic diffusion region. In order to study the three-dimensional instability of the fast magneticreconnection, we developed a multi-scale MHD simulation code in which the magnetic diffusion region issimulated in a high- resolution MHD code and the other regions are simulated in a macro-scale MHD code. As anapplication of this new code, the self-organization of three-dimensional pulsive fast magnetic reconnection ispresented in this paper.

P3-055

The Seasonal and Solar Cycle Variations of Electron Density Gradient ScaleLength and F Layer Vertical Drift during Magnetically Disturbed DaysG. Manju, C. V. Devasia, and Sudha Ravindran

SPL

A study has been carried out on the behaviour of electron density gradient scale length, L and vertical drift at ~1900 hr during the magnetically disturbed days of summer, winter and equinox seasons of solar maximum (2002)and minimum years (1995), using ionosonde data of Trivandrum (8.5 N, 76.5 E, dip = 0.5 N) in the Indianlongitude sector. The results indicate a clear seasonal and solar cycle variation in L and vertical drift both for solarminimum and maximum. Substantial reduction in the vertical drift is observed during magnetically disturbed daysof equinox and winter in both the solar epochs in comparison with the behavior during magnetically quiet period.For the magnetically disturbed days of summer the vertical drift shows a small reduction during solar maximumand an increase during solar minimum in comparison with the corresponding magnetically quiet period. Theseasonal variation of equatorial Spread F (ESF) during the above period is examined in terms of the relative rolesof L and the vertical drift of the F layer in the triggering of the Rayleigh-Taylor instability.

- 182 -

P3-056

Origin of Weak and Moderate Geomagnetic StormsOlga Khabarova

Space Research Institute (IKI), 84/32 Profsoyuznaya Str, Moscow, Russia

The question "What is geomagnetic storm?" is debated by many years, but quality of geomantic storms' predictionis very low till now. Statistical and case-study investigations of magnetic storm's origin, which able to improveprognostic accuracy are discussed.

P3-057

Observations of Space Weather Events from the Sun to the EarthIonosphere and ThermosphereChristian Hanuise1 and PNST team2

1. LPCE/CNRS, 3A av. de la Recherche Scientifique, 45071 Orleans Cedex, France2. IAS, Bat. 121, Universite Paris Sud, 91405 Orsay Cedex, France3. CETP, 10-12 av. de l'Europe, 78140 Velizy-Villacoublay, France4. CETP, 4 av. de Neptune, 94107 St Maur des Fosses Cedex, France5. CESR/CNRS, 9 av. du Colonel Roche, 31028 Toulouse Cedex 4, France6. LPG, BP 53, 38041 St Martin d'Heres Cedex 9, France7. LESIA, Observatoire de Paris, 92195 Meudon Cedex, France8. ESTEC, RSSD, Postbus 299, 2200 AG Noordwijk, The Netherlands9. DMI, Lyngbyvej 100, 2100 Copenhagen, Denmark

Solar events and their impact on the terrestrial environment have received a lot of attention in recent years.Nevertheless, the relations between the solar source and their effects in the terrestrial environment are far frombeing understood quantitatively let it be for the physical mechanisms (solar-terrestrial physics) or for the effectson living bodies and technological systems (space weather). Are successively involved the formation mechanismof solar flares and Coronal Mass Ejections (CME), the propagation within the solar wind, the interaction with theEarth magnetosphere and the coupling between the magnetosphere, the ionosphere and the neutral atmosphere.The large number of ground-based and space-borne instruments presently in operation allows one to follow theperturbations at various locations along their path: the Sun (photosphere, chromosphere, corona), L1, the interfacebetween the solar wind and the magnetosphere, the inner magnetosphere, the ionosphere and the thermosphere. Asa first step, we have focused our attention on a case study in May 2003 for which a moderate solar activity had astrong impact at Earth. It has been possible to follow the origin of the Coronal Mass Ejections, the presence ofinterplanetary shocks and magnetic clouds passing the ACE satellite, the strong compression of the

- 183 -

magnetosphere unto five Earth radii, and a strong magnetic storm with numerous manifestations of adverse spaceweather.In order to progress in the understanding of the physical processes and of the coupling between adjacent regions,one sensible approach is to define proxies at a limited number of locations along the path from the Sun to theEarth. Some of these proxies already exist, as for example the solar flare magnitudes, at e.g. optical or X-raywavelengths, or the magnetic indices, but this is not the case in all important regions. Other proxies should alsorepresent the compression of the magnetosphere, the response of the ionosphere, the state of the thermosphere, theradio absorption and other space weather manifestations. We present possible candidates and examine theirbehaviour during a limited number of space weather events. Once the proxies have been defined, they can be usedas tools for comparing various events. For example, what is the response of each proxy as a function of eventintensity, what is the cause of differences in their relative responses, or what is their statistical behaviour? Thiswill help in understanding the physical processes involved, in defining tools for space weather events and inreaching the ultimate goal of an integrated Sun-Earth connection science.

P3-058

Contributions to CAWSES through the Geospace Research Center Project2: Initiatives in Geospace Research Using Coordinated Ground-satelliteExperimentsKazuo Shiokawa , Satonori Nozawa, Kanako Seki , Yoshizumi Miyoshi , and Nozomu Nishitani

Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, 464-8601, Japan

Geospace is the closest space region for human beings, where artificial satellites and space stations exist. Geospace research center of the Solar-Terrestrial Environment Laboratory, Nagoya University initiated three5-year projects from April 2004. The project 2 (Initiatives in geospace research using coordinated ground-satelliteexperiments) aims to elucidate the nature of the energy/mass transport in the geospace region that includes themagnetosphere, ionosphere, and thermosphere, by coordinating new experiments from ground and satellites. During 2004-2007, project 2 have supported the following research activities: 1) airglow/aurora measurements attwo stations in Canada (Resolute Bay at 83 MLAT and Athabasca at 62 MLAT), 2) feasibility study of thesatellite mission ERG (Energization and Radiation in Geospace) to investigate the dynamics of the innermagnetosphere, 3) investigation of particle and field structures at auroral substorm onset using the DMSPsatellites and ground all-sky cameras, 4) ground-satellite measurements of aurora and ion upflow using the Reimeisatellites and the EISCAT radar and aurora imagers, 5) ground-satellite measurements of front-like structure in themesosphere at geographic equator using the TIMED satellite and a ground airglow imager, 6) installation of a newSuperDARN HF radar at Rikubetsu, Japan, 7) installation of a new meteor radar at Bear Island, Norway, and 8)optical and riometer measurements of the ionosphere near the geomagnetic anomaly region in Brazil and Chile.

- 184 -

P3-059

Inferring the Ionospheric Global Potential Distribution from SuperDARNData through the IMech Numerical ModelMonio Kartalev1, Ermanno Amata2, Igino Coco2, Valentina Keremidarska1, and Vladimir Papitashvili3

1. Institute of Mechanics, Bulgarian Academy of Sciences2. Istituto di Fisica dello Spazio Interplanetario, INAF, Roma, Italy3. Space Physics Research Laboratory, University of Michigan, Ann Arbor, Michigan, U.S.A

An attempt for a new implementation of the IMech numerical model of the global ionospheric electric potentialdistribution is presented. The 2D spherical thin shell approach used in this model is obtained reducing the 3Dapproach of the electrodynamics problem, posed in coordinate system, aligned with the geomagnetic field andbased on realistic global conductivities distributions. The model comprises the global computational region, whichincludes both conjugate ionospheres as separate sub-domains. Field-aligned currents between magneticallyconjugate points (with not necessarily equal potentials) are permitted. The model is really global, includingtogether high, middle, and low latitudes. The special role of the equatorial ionosphere is obtained as a part of theglobal model. Consideration of different driving sources of the ionospheric potential distribution is possible,including currents with solar wind and magnetosphere origin, acting over both - the northern and southern polarregions; dynamo effects of the thermal and gravitational tides in the thermosphere; atmospheric electricity effects.We discuss here the possible implementation of the potential distributions calculated simultaneously at bothhemispheres from SuperDARN data through the JHUAPL model as an input to the global model. A modificationof the IMech Ionospheric Electrodynamic Model may be used for converting SuperDARN potential distributionsinto distributions of the polar field aligned current system in both hemispheres, becoming in this way inputs,needed by the global model. The result is a self-consistent global potential distribution.

P3-060

Vertical Wind Observation in the Tropical Upper Troposphere by VHFWind Profiler - A Case Study -Masayuki K. Yamamoto1, Takeshi Horinouchi1, Masanori Niwano2, Noriyuki Nishi3, Mamoru Yamamoto1, Hiroyuki Hashiguchi1, and Shoichiro Fukao1

1. Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Japan2. Frontier Research Center for Global Change, Japan Agency for Marine-Earth Science and Technology, Yokohama, Japan3. Division of Earth and Planetary Sciences, Graduate School of Science, Kyoto University, Kyoto, Japan

Features of upper-tropospheric vertical wind (W) over Sumatra, Indonesia are presented using data observed byVHF wind profiler (Equatorial Atmosphere Radar; EAR) installed at West Sumatra (0.2degS, 100.32degE).During 5-9 May 2004, W from the middle to upper troposphere (8-14 km) changed in accordance with thecumulus activity over Sumatra. During 5-6 May, 3-hourly averaged W continuously showed upward motions upto about 0.09 m/s. The upward motions were observed in the vicinity of deep convective events, which werecontinuously seen over Sumatra within a synoptic-scale convectively active envelope. After 7 May, when cumulusactivity was suppressed over Sumatra, 3-hourly averaged upward motions of greater than 0.05 m/s almostdisappeared. During 5-6 May, downward motions up to about 0.11 m/s were observed above 14 km, while upward motionswere observed below 14 km. Estimation of W by the ECMWF operational analysis have revealed that a major partof observed downward motions above 14 km is explained by the leeward (southwestward) wind and leewarddownward tilt of isentropes existed over the western Sumatra.The observed downward motions above 14 km during 5-6 May suggest that downward motions caused by leewarddownward tilt of isentropes can be produced in the vicinity of convectively active region, and leeward downwardtilt of isentropes can suppress an upward transport of airmass into the tropical tropopause layer (TTL) byproducing downward motions in the TTL.

- 185 -

P3-061

Gravity Wave Momentum Fluxes in the Middle Atmospheric Region(30-100km) and Their Role in Driving the SSAO/MSAOT. Maria Antonita, Geetha Ramkumar, Karanam Kishore Kumar , and V. Deepa

Space Physics Laboratory, Vikram Sarabhai Space Center, Thiruvananthapuram, India.

Atmospheric science community unanimously concurs the profound role played by gravity waves in the verticalcoupling of the different regions of the Earth's atmosphere. Divergence/convergence of the energy and momentumfluxes carried by the gravity waves accelerate/ decelerate the mean flow which in turn partly responsible for themaintenance of Quasi Biennial Oscillation (QBO), Stratospheric Semi Annual Oscillation (SSAO) andMesospheric Semi Annual Oscillation (MSAO), which are the characteristic features of the equatorial middleatmosphere. Rayleigh lidar observations of middle atmospheric temperature over Gadanki and Rocketsonde windmeasurements over Trivandrum, under ISRO's Middle Atmospheric Dynamics (MIDAS) program are used toestimate the gravity wave momentum fluxes and their forcing towards SSAO during November 2002- June 2005.The altitude profiles of momentum fluxes of gravity waves (periods ranging from 2-4 hr and 0.5-1 hr) areestimated and their seasonal variations are studied. The mean flow acceleration estimated from the divergence ofgravity wave momentum fluxes is compared with the mean flow acceleration observed using rocket measuredzonal winds during three different cycles of SSAO. In the MLT region, gravity wave momentum fluxes (2-3 hr)estimated from meteor radar observations are used to quantify their contribution towards the easterly and westerlyphases of six MSAO cycles during June 2004- May 2007. The significance of the present study lies in estimatingthe gravity wave momentum fluxes in the middle atmospheric region and quantifying their contributions indriving the SSAO and MSAO over the low latitude for the first time.

P3-062

Multi-technique Study of the Solar Wind-Magnetosphere-IonosphereCoupling Effects into the Equatorial and Low-latitude Ionosphere in theIndian Region.D. Tiwari1, B. Kakad1, S. Sripathi1, M. Yadav1, T. K. Pant 2, A. K. Patra 3, and A. Bhattacharyya1

1. Indian Institute of Geomagnetism, New Panvel, Navi Mumbai-410 218.2. Space Physics Laboratory, VSSC, Trivandrum-695022.3. Atmospheric Research Laboratory, P O Box: 123, Tirupati-517502.

An important effect of geomagnetic activity, as far as communication/navigation systems are concerned, is thegeneration of Equatorial Spread F (ESF) irregularities and evolution of spatial structure in them. The present studyinvestigates the evolution of irregularities in the equatorial and low-latitude ionosphere under different ambientconditions in the Indian longitude sector with the existing network of single/spaced receiver VHF scintillationexperiments, Ionosondes and the Indian MST radar. Observations of ESF irregularities made using the Indian MST radar located at Gadanki (13.50 N, 79.20 E, Diplatitude 6.30 N), simultaneous observations of scintillations on a VHF signal transmitted from a geo-stationarysatellite and recorded at Tirunelveli (8.70 N, 77.80 E, Dip latitude 0.60 N) and Mumbai (19.090 N, 72.850 E, Diplatitude 13.60 N) and Ionosonde observation at Trivandrum (8.50 N, 770 E, Dip latitude 0.50 N) are reported. Oneof the shortcomings of using the technique of ionospheric scintillation and radar backscatter in studying the effectof solar wind-magnetosphere-ionosphere coupling on the generation of ESF irregularities is that it is not knownwhether the observed irregularities are freshly generated or were generated earlier at some location to the west ofthe observation point and then simply drifted overhead at a later time. Some effort has been made to study thisissue using VHF scintillation and MST radar observations. Spaced receiver scintillation observations of ESF irregularities at Tirunelveli and their association with Ionosondemeasured parameters have also been investigated for magnetically quiet and disturbed days.

- 186 -

P3-063

Dynamical Coupling Processes in the Equatorial MiddleAtmosphere-Results from ISRO MIDAS ProgramGeetha Ramkumar1, KVS Namboodiri2, Debadatta Swain3, Sunil Kumar3, Maria Antonita3, and Bhavani Kumar3

1. Space Physics Laboratory, VSSC, ISRO, Trivandrum, India,695 0222. MET Facility, VSSC, ISRO, Trivandrum, India,695 0223. National Atmospheric Research Laboratory, Gadanki, India

A five year long ISRO Middle Atmosphere Dynamics Program MIDAS (2002-2007) is running successfully, withmultiple scientific objectives and these objectives are exactly fitting into theme III of CAWSES program.It is well known that the equatorial middle atmosphere hosts a wide range of dynamical processes which arecoupled with lower, middle and upper regions of the earth atmosphere. It is also observed that equatorial processesare influenced by some high latitude phenomena like sudden stratospheric warming (SSW).Under MIDAS program, co-ordinated measurements of winds and temperatures are made fortnightly and oncampaign basis, using Balloon flights, RH 200 rocket flights, Partial Reflection Radar and Meteor wind radarmeasurements from Trivandrum (8 N) and MST Radar and Lidar measurements at NARL, Gadanki (13.5 N). Themonthly mean values of temperature and horizontal winds in the TSM region were derived from the data collectedduring 2002-2007 and these were used to study the QBO and SAO throughout the middle atmospheric region. Theyear to year variation and cycle to cycle variation of these oscillations and the relationship between QBO, SSAOand MSAO will be presented in detail.Analysis of wind and temperature data at tropical latitudes, from surface to 100 km, obtained from a 20 day longcampaign mode of observations during 20 January-8 February 2006, (covering a major SSW event) could revealdistinctly different changes in temperature and circulation at different levels within 2-4 days of peak warmingevent. The strong and sudden thermal perturbations may have implications in the radiative, dynamical andchemical processes of the middle atmosphere.

P3-064

Precipitating Clouds over Kototabang, West Sumatra Observed by WindProfilersHiroyuki Hashiguchi1, Findy Renggono2, Masayuki K. Yamamoto1, Toshiaki Kozu3, Toyoshi Shimomai3, and Shoichiro Fukao1

1. Research Institute for Sustainable Humanosphere (RISH), Kyoto University, Japan2. Agency for the Assessment and Application of Technology (BPPT), Indonesia3. Department of Electronic and Control Systems Engineering, Shimane University, Japan

The occurrence of deep convection in the tropics affects the global circulation, since it transports the heat fromatmospheric boundary layer to the upper troposphere. Since the vertical distribution of diabatic heating dependson the vertical structure of the convective system, it is important to study the vertical structure of the precipitatingclouds occurring in the tropics. The diurnal variability of DSD in precipitating clouds over Kototabang (0.2S,100.3E) in West Sumatra, Indonesia is studied using three types of Doppler radars, operated at VHF- (47 MHz),UHF- (1.3 GHz), and X-band (9.4 GHz) frequencies. Two precipitating events from 5 to 6 May 2004 in the firstobservation campaign of the Coupling Processes in the Equatorial Atmosphere (CPEA) project reveal thedifference between precipitating clouds in the early afternoon and the nighttime. In the early afternoon theprecipitating clouds are dominated by shallow convective types with high rainfall rate at the surface. In thenighttime precipitating clouds are dominated by stratiform types with small rainfall rate. DSD parameters areretrieved from a VHF-band Equatorial Atmosphere Radar (EAR). A modified gamma distribution is used tomodel DSD parameters. The shape parameter is larger during stratiform precipitation than during shallowconvective precipitation events. During stratiform rain events on 5 May 2004 the median volume diameter (D0) isaround 1 mm, which is larger than D0 during shallow convective rain events. Results presented in this studyindicate that DSD has a diurnal cycle over the mountainous region of Sumatra.

- 187 -

P3-065

Study the Short Period Gravity Waves in the Indian Tropical MiddleAtmosphere and Associated Momentum Flux Using Indian MST RadarN.Y.Pandya, H P joshi, and K N iyer

Department of Physics, Saurashtra University Rajkot-360005

Atmospheric Gravity waves have been a subject of intense research activity in recent year because of their myriadeffects and their major contributions to atmospheric circulation, structure and variability. Gravity waves also playvery important role in carrying energy & momentum from lower to middle atmosphere and hence in couplingbetween troposphere and stratosphere. MST radar observations for a number of days during the months of July,August, October, November, December, January, February, April from 2001 - 2005 are used for the present studywith time resolution is 4 minutes and height resolution 150 m. The zonal, meridional and vertical componentare derived from the Doppler spectra. The mean zonal wind is mostly eastward during winter, reaching maximumvalue at 15 m/s at a height of about 12 to 17 km and mean zonal wind is mostly westward during July, Augustreaching maximum ~30 m/s at a height of 12 to 18 km .The prominent peaks of the variance are seen between ~14 km and ~ 16km. Zonal momentum flux varies from -0.8 to -0.4 m2/s2 and meridional momentum flux isvaries form -0.3 to 0.3 m2/s2. The height-time structure of the periodicities obtained from the FFT analysis. Thedominant period of the wave like structure is found to be in the range of the 20 to 40 min. Wavelength inferredfrom hodograph is ~5 to 6 km.

P3-066

Seasonal Variations of Ultra-fast Kelvin Waves Observed in the EquatorialMesosphere and Lower Thermosphere over TirunelveliS.Sathishkumar and S.Gurubaran

Equatorial Geophysical Research Laboratory, Krishnapuram, Tirunelveli-627011. India

The medium frequency (MF) radar has been used to measure the mean winds and planetary waves at heights of70-98 km in the mesosphere and lower thermosphere over Tirunelveli (8.7&#61616;N, 77.8&#61616;E) in theequatorial latitude. The wave periods varying from 3-4 days are generally called ultra-fast Kelvin (UFK) waves.The Kelvin wave is one of the most dominant equatorially trapped modes in the tropical atmosphere. In thepresent work, we have analyzed the MF radar data for the year 2005 to study the characteristics and seasonalvariability of 3.5 day ultra fast Kelvin wave. It was observed that 3.5 day wave activity was dominating duringsecondary westward phase of mesopause semiannual oscillation (MSAO). The enhancement of wave activity isdue to westward flow regimes of the back ground wind flow. The preliminary result suggests that the UFK waveexhibits the intraseasonal variations in the equatorial MLT region. The detailed analysis is being carried out andthe results will be presented.

- 188 -

P3-067

Energetic Particles Coming from Space and Their Role for Short/Long - Term Changes in the Atmosphere of the EarthAlexei Krivolutsky

Central Aerological Observatory, Dolgoprufny, Moscow Region Russia

Energetic particles (EPs): solar and galactic cosmic rays, and precipitating electrons, which penetrate into theatmosphere of the Earth at high latitudes, cause its ionization and transform chemical composition includingozone. Ozone response, which is caused by additional production of nitrogen and hydrogen oxides in the middleatmosphere, depends of magnitudes of particle fluxes and its energetic spectrum. During the deceleration in theatmosphere each pair of produced ions born 1.25 molecular of NO and 2.0 molecular of OH (Porter et al, 1976;Solomon and Crutzen, 1981), which destroy ozone in chemical catalytic cycles. Increase of hydrogen compoundsleads usually to short term effects in the atmosphere, and NOx production by energetic particles induces long-termconsequences. EP-induced changes in ozone transform radiative fluxes in the atmosphere, and so transformtemperature and winds (Krivolutsky et al., 2006). This conception was used in order to investigate the response of the atmosphere to major SPEs of solar activity23-rd cycle. Middle atmosphere GCM (COMMA/CAO) and 3D transport photochemical model has been used forsuch study (Krivolutsky et al., 2006). Changes in ozone structure during and after SPEs has been incorporated intoradiative module of GCM for each SPE disturbing temperature fields and circulation. The results of 3D simulations showed that major SPEs caused strong depletion in ozone at high latitudes,transform temperature and wind fields. Changes in zonal wind penetrate to the lower latitudes. It was shown alsoin model runs that lower atmosphere has the sensitivity to such short-term external forcing during the periods oflarge-scale planetary wave activity. Long-term effects were studied on the basis of data analysis.

ReferencesKrivolutsky A. et al., Dynamical response of the middle atmosphere to solar proton event of July 2000: Threedimensional model simulations, Advances in Space Research, 37, 1602-1613, 2006.Solomon, S. and P. Crutzen, Analysis of the August 1972 solar proton event including chlorine chemistry, J.Geophys. Res., 86, 1140-1151, 1981.Porter, H. S., C. Jackman, A. E. S. Green, Efficiences for production of atomic nitrogen and oxygen by relativisticproton impact in air, J. Chem. Phys., 65, 154, 1976

- 189 -

P3-068

Reanalysis of Greenline Dayglow Emissions with Different Solar EUV FluxModelsArun Kr. Upadhayaya

Department of Physics, 580 Delhi-Palam Vihar Road, Bijwasan, Amity School of Engeenering & Technology, New Delh i-110061 India

A key problem in the modeling of dayglow is the appropriate use of solar extreme ultra violet (EUV) flux. Thesesolar EUV flux are involved in direct and indirect processes of excitation of atmospheric species which accountsfor the production of airglow emissions. Hinteregger et al.(1981), Tobiska (1991) and Solar (2000) model are themodels that provides solar EUV flux. These models provide the solar fluxes under different solar activitycondition having quite different scaling technique. An exercise has been done to test the efficacy of these solarEUV flux models. In this study a reanalysis of greenline dayglow emission profile between 120 -250 km measured by WINDII on board the Upper Atmosphere Research Satellite (UARS) in the light of proposedtemperature dependence of the rate coefficient for the reaction N2(A3+) with O using the Glow model. TheVolume Emission rates (VER) of the greenline dayglow emission are calculated using different solar EUV fluxmodels using quantum yield of 0.36.

P3-069

Characteristics of Atmospheric Waves in the Equatorial RegionToshitaka Tsuda1, Simon P. Alexander1, Yukari Takayabu2, Toshiaki Kozu3, and M. Venkat Ratnam4

1. Research Institute for Sustainable Humanosphere (RISH), Kyoto University2. Center for Climate System Research (CCSR), University of Tokyo3. Faculty of Science and Engineering, Shimane University4. National Atmospheric Research Laboratory (NARL)

Active cumulus convection in the tropics generates various waves, such as Kelvin waves, tides, gravity waves, etc.The upward propagating waves are crucially important for the understanding of dynamical processes in theequatorial atmosphere, including the formation of peculiar long-term variations such as quasi-biennial oscillation(QBO) and semi-annual oscillation (SAO) in both the stratosphere and the MLT (mesosphere and lowerthermosphere) region (70-120 km). In order to continuously measure wind velocity in the MLT region, we operateMF and meteor radars in Indonesia since 1992. The equatorial atmosphere radar (EAR) installed in 2001 monitorswinds in the troposphere and lower stratosphere. We also repeated a number of intensive campaigns with radiosondes to measure wind velocity and temperatureprofiles at 0-35 km. In addition, we employ satellite data, such as GPS radio occultation (RO) data with CHAMP,SAC-C and COSMIC stellites, as well as TRMM-PR results. We discuss in this paper the behavior of atmosphericwaves in the tropics from intensive radiosonde campaigns, radar observations and satellite data.

- 190 -

P3-070

Development of the Whole Atmosphere and Ionosphere Vertical CouplingModelHidekatsu Jin1, Yasunobu Miyoshi2, Hitoshi Fujiwara3, Hiroyuki Shinagawa1, Mamoru Ishii1, Yuichi Otsuka4, and Akinori Saito5

1. National Institute of Information and Communications Technology2. Kyushu University3. Tohoku University4. Solar-Terrestrial Environment Laboratory, Nagoya University5. Kyoto University

Recent atmospheric and/or ionospheric observations have increased the importance of understanding the verticalcoupling processes between the atmosphere and the ionosphere. Even during geomagnetically quiet periods,day-to-day variability of ionospheric phenomena (e.g., EIA and plasma bubble) was observed by ground-basedinstruments. Their seasonal and longitudinal dependences were also observed by spacecraft instruments. Suchvariations in the ionospheric phenomena are believed to be affected by atmospheric variations though theatmospheric dynamo process. In fact, there have been some observations in recent years, which suggest a closerelationship between the atmospheric waves originated in the lower atmosphere and the ionospheric variations. Instorm time, moreover, atmosphere-ionosphere interactions are considered to play an important role in causing theobserved ionospheric/atmospheric disturbances; behaviors of TID/TAD, effects of change in the atmosphericcomposition and neutral wind circulation, and so on. These observations have made the role played by numericalmodel which couples the atmosphere and the ionosphere more important.Development of regional coupling models is now very active, such as TIME-GCM (NCAR) for the upperatmosphere and the ionosphere, and CISM and SWMF for the whole geospace. In Japan, thetroposphere-stratosphere-mesosphere-thermosphere GCM has been developed in the university of Kyushu andTohoku, and the thermosphere-ionosphere model developed in NICT, independently. In this project, we willdevelop vertical coupling model between the atmospheric regions and the ionosphere by coupling the two modelsand adding the atmospheric dynamo process. In this presentation, we will report the outline of our project and thefirst results.

- 191 -

P3-071

All-sky Imaging Observations of Prominent Mesospheric Gravity WaveEvents over Tirunelveli (8.7N, 77.8E)V. Lakshmi Narayanan, S. Gurubaran, and K. Emperumal

Indian Institute of Geomagnetism, India

Observations of airglow emissions provide important information about the dynamics of the region from whichthey emanate. Ground based optical imaging observations of equatorial mesospheric airglows are relatively lesscompared to those in the high latitudes. Recently, a multi-wavelength all-sky airglow imager has been installed atthe equatorial site Tirunelveli (8.7N, 77.8E; 0.73N dip latitude), India. The imager is equipped with threeinterference filters to observe mesospheric emissions from hydroxyl radical (710-920 nm, filter with a notcharound 865 nm), sodium (589.3 nm) and green line of atomic oxygen (557.7 nm). In addition to the all-skyimager, an MF radar operated at this site provides valuable information on winds at heights where hydroxylemission originates. In this paper we examine a few prominent quasi-monochromatic wave features present in theairglow images.

P3-072

Longitudinal Variabilities of the Diurnal Tide in the Low LatitudeMesosphere-Lower Thermosphere (MLT) RegionS. Gurubaran1, S. Sridharan2, T. Nakamura3, T. Tsuda3, H. Takahashi4, P. P. Batista4, B. R. Clemesha4, R. A. Buriti5, D. V. Pancheva6, and N. J. Mitchell6

1. Equatorial Geophysical Research Laboratory, Indian Institute of Geomagnetism, Tirunelveli, India2. National Atmospheric Research Laboratory, Gadanki, India3. Research Institute for Sustainable Humanosphere, Kyoto University, Kyoto, Japan4. Instituto Nacional de Pesquisas Espaciais, Sao Jose dos Campos, Brazil5. Departmento de Fisica, Universidade Federal de Campina Grande, Brazil6. University of Bath, Bath, UK

Vertically propagating tides carry significant amount of energy and momentum into the mesosphere-lowerthermosphere (MLT) region. Wave damping processes operate at these heights efficiently along with waveinstabilities that together account for the transfer of energy and momentum from the dissipating diurnal tide intothe background atmospheric region. Apart from modulating the background flow through which other wavecomponents propagate, the tides do interact non-linearly with planetary waves and gravity waves therebycontributing to their variabilities. An active area of current research lies in understanding the tidal variabilities andassociating them with the variations in the known sources of tidal origin.The present work makes use of a low latitude network of MLT radars at four sites: Cariri (7.4S, 36.5W),Ascension Island (7.9S, 14.4W), Tirunelveli (8.7N, 77.8E) and Pameungpeuk (7.7S, 107.7E). The locations ofthese sites are well suited for examining the longitudinal variabilities of the diurnal tide in the low latitude MLTregion. Simultaneous wind observations from the above four sites are utilized for the period June 2004-December2005 in order to delineate the longitudinal differences in the tidal amplitudes and phases. Both monthlycomposites and 5-to-10-day composites of hourly winds are used in the analysis to examine the long-term (inseasonal time scales) and short-term variabilities of diurnal tide over these sites. A rigorous analysis has been

- 192 -

performed to bring out the wavenumber characteristics of the dominant mode. The differences in the tidalcharacteristics are discussed in the context of our present understanding of tidal forcing mechanisms and thevarious aspects related to the tidal propagation in the equatorial middle atmosphere.

P3-073

Interaction between Stratosphere and Troposphere on Quasi-biennialTimescale Linked with Indian Summer MonsoonPrasanth A Pillai and K.Mohankumar

Department of Atmospheric Sciences, Cochin University of Science and Technology, Cochin-682 016, Kerala, India

Quasi-biennial oscillation (QBO) is a predominant phenomenon in the tropical stratospheric zonal winds.QBO-type oscillation is also observed in the troposphere and is termed as tropospheric biennial oscillation (TBO).TBO is evident in tropospheric winds, SST, precipitation etc over the tropical region. In the present study, thepossible interaction between the stratospheric QBO and TBO in the tropics is investigated. ECMWF zonal windand temperature data from 1000 hpa to 1 hpa and NCEP SST and Indian summer monsoon rainfall data from1960-2002 periods have been used. These data are filtered to retain the biennial time scale. Biennial periodicity isthe most prominent oscillation for the stratospheric winds. Whereas in the troposphere, annual cycle and ENSOtime scale variations are also important along with biennial periodicity. Zonal winds in the stratosphere havedownward propagation with constant speed, while the zonal winds at the different levels of the troposphere exhibiteastward propagation. This eastward propagation is also noted for tropical SST and is a basic property of TBO. Inthe equatorial region, the downward propagating stratospheric winds and the upward propagating troposphericwinds meet at about 100 hpa level, near the tropopause. A dipole like structure is observed in the zonal windstructure with westerlies in the lower troposphere and easterlies in the upper troposphere during the period ofstrong TBO monsoon and reverse is seen for weak TBO monsoon. Over the Indian monsoon area, the upwardpropagation of the lower level winds is absent during the TBO years and the stratospheric winds extends deepdownwards in to the troposphere. In the TBO years the winds in the troposphere and stratosphere are also relatedwith tropical SST. The winds at different levels of the troposphere over the Indian monsoon region have shownsignificant lag correlation with QBO index. Similar type of relationship is also obtained for temperature. Thepresent study indicates that the stratospheric QBO and the tropospheric biennial oscillation have got a strong

- 193 -

association with the Indian summer monsoon.

P3-074

Study of the Response of the Equatorial Ionosphere-Thermosphere to theSpace Weather Events : Results from the CAWSES India CampaignTarun Kumar Pant1, C.Vineeth1, Smitha Thampi1, V. Sreeja1, G. Manju1, S. Banola2, Diwakar Tiwari2, Sudha Ravindran1, C.V.Devasia 2, Harish Chandra3, and R.Sridharan 1

1. Space Physics Laboratory, Vikram Sarabhai Space Centre, Trivandrum, India2. Indian Institute of Geomagnetism, Navi Mumbai, India3. Physical Research Laboratory

Under the aegis of CAWSES, one multi-instrument campaign was conducted in India during March-April 2006.One aim of the campaign was to understand the processes vertically coupling the Mesosphere, LowerThermosphere and Ionosphere (MLTI) regions over the low and equatorial latitudes. A Multiwavelength dayglowPhotometer (MWDPM) was operated along with ionosonde and magnetometer from Trivandrum (8.5oN, 76.5oE,0.5oN diplat.), the dip equatorial station in India; and a ground-based chain of TEC and scintillation receiversfrom stations across India. The MWDPM provided measurements on the thermospheric dayglow (O1D 630 nm)emission intensity near simultaneous to the ionospheric measurements. Overall, the TEC and the thermospheric dayglow measurements reveal significant day-to-day variability whichcan be understood in terms of the development and evolution of the Equatorial Ionisation Anomaly (EIA).However, their variations on some days were found to be rather unusual and intriguing. For instance, the emissionintensity on March 30 and 31 showed a prominent decrease during 1400-1600 IST (Indian Standard Time i.e.UT+5.5). On the contrary, March 29 exhibited an increase (> 30%) during 1300-1400 IST. Further, on some daysstrong daytime scintillations in L-band were observed at off-equatorial latitude followed by generation of ESF inthe post-evening hours as inferred from the ionosonde over the dip equator. The nighttime tomographicreconstructions of the ionospheric density reveal the presence of Traveling Atmospheric Disturbances on some ofthese days. These observations will be presented and discussed in context of the MLTI coupling, especially over equator and

- 194 -

low latitudes.

P3-075

Electrodynamics of the Equatorial F region Ionosphere during Pre-sunrisePeriodTiju Joseph Mathew1, C.V. Sreehari1, S. G. Sumod1, S R Prabhakaran Nayar1, C V Devassia2, Sudha Ravindran2, Tarun Pant2, V.Sreeja2, and R.Sridharan2

1. Department of Physics, University of Kerala, Trivandrum 695 022, India2. Space Physics Laboratory, Vikram Sarabhai Space Centre, Trivandrum 695 022, India

The vertical plasma drift at the equatorial F region during post sunset and pre-sunrise periods are primarily drivenby a zonal electric field formed as a part of the polarization electric field developed due to the thermospheric windand the decay of E region conductivity. Though the ionosphere during the evening hours has been well explored,the pre-sunrise phenomena are not yet studied in detail. The present study investigates this very aspect of thenighttime equatorial ionosphere. A multi-frequency HF Doppler radar located at the magnetic equatorial station,Trivandrum (8.5°N, 76.5°E) working at three fixed frequencies - 2.5 MHz, 3.5 MHz and 4.5 MHz has been usedfor this study. For most of the days, the sounding of the ionosphere during the early morning hours was notpossible due to the fall in the foF2 values below these probing frequencies. The vertical drift data observed usingthe HF Doppler radar is compared with that estimated using Trivandrum ionosonde. Since the observed verticaldrift is the sum of the electrodynamic drift and an apparent drift due to the photochemical production, theobserved vertical drift using both ionosonde and HF Doppler radar are modified by applying appropriatecorrection due to photochemical production. The observed vertical drift profiles during the pre-sunrise period havethree major characteristics - (i) an upward enhancement in the vertical velocity occurring around 05:00 to 06:00LT, prior to the ground sunrise, (ii) it is followed by a sharp downward fall during 06:00 - 06:30 LT and (iii) anupward turning beyond 06:30 LT. The day-to-day variations of the vertical plasma drift reveal this to be a typicalfeature of the pre-sunrise equatorial F region. The observed pattern in vertical plasma drift is in agreement withthat predicted by Farley's model. These observations will be presented and discussed in detail.

- 195 -

P3-076

Numerical Investigation on Spontaneous Gravity Wave Radiation from a JetStream in a Simplified ModelNorihiko Sugimoto1 and Katsuya Ishii2

1. Graduate School of Engineering, Nagoya University, Nagoya, Aichi 464-8601, JAPAN2. Information Technology Center, Nagoya University, Nagoya, Aichi 464-8601, JAPAN

We study spontaneous gravity wave radiation from a jet stream in a shallow water system on a rotating sphere. Itis well known that gravity waves play an important role on the middle atmosphere to drive a global circulation.Recent observational studies suggested that gravity waves are radiated from strong rotational flows, such as polarnight jet. In the present study, we focus on one radiation mechanism, in which gravity waves are spontaneouslyradiated from initially balanced rotational flows. For the numerical simulation we use the spectral-like three pointcombined compact difference (sp-CCD) scheme, which has high accuracy as well as the spherical harmonicsmodel. This model allows us to estimate gravity wave amplitude with high accuracy. We make an unsteady jetflow with zonal relaxation forcing. Then spontaneous gravity wave radiation is generated continuously. Thelatitudinal dependencies of the jets on spontaneous gravity wave radiation are investigated. Using the analogywith the theory of the aero-acoustic sound wave radiation (Lighthill theory), we discuss on the conditions ofgravity wave radiation and propagation. We also discuss results with the basis of f-plane shallow water systemwhich we studied previously. In addtion, we will show recent results in two-layer system.

P3-077

Quasi Biennial Oscillation of the Stratospheric Background AerosolObserved by Lidar over the Equatorial RegionMakoto Abo, Chikao Nagasawa, and Yasukuni Shibata

Faculty of System Design, Tokyo Metropolitan University, Hino, Tokyo 191-0065, Japan

Stratospheric aerosol layers have been almost in steady state since the eruption of Mt. Pinatubo in 1991. Theresults of our stratospheric lidar observation at Kototabang in the equatorial region show that the stratosphericaerosol layers in mid-latitude are usually lied from tropopause to about an altitude of 30km, but at Kototabang,those are seen from tropopause (16-18km) to around 40km. In April 2004, top height is about 40km, but itdecrease slowly. The descending rate is seemed to be synchronizing with the phenomenon of QBO. In addition,there is much troposphere aerosol around the tropopause in the equatorial region in comparison with themid-latitude. We can regard this as evidence of atmospheric exchange between troposphere and stratosphere.

- 196 -

P3-078

Effects of TADs on the F Region of the Mid-latitude Ionosphere duringGeomagnetic StormsZhigang Yuan1, Baiqi Ning2, and Xiaohua Deng1

1. School of Electronic Information, Wuhan University, Wuhan, 430072, P. R. China2. Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, P. R.China

Based on observations of two ionosondes at Wuhan and Kokubunji, this paper presents effects of an intensegeomagnetic storm on the daytime mid-latitude ionosphere on March 31, 2001. During a positive ionosphericstorm, the start of the enhancement of the foF2 (F2 peak plasma frequency) at Wuhan lags that at Kokubunji by 15min, which corresponds to the time interval of traveling atmospheric disturbances (TADs)' propagation fromKokubunji to Wuhan. Associated with the uplifting of the hmF2 (height of F2 peak), it is observed by the twoionosondes that the F1 cusp becomes better developed. Therefore, during a geomagnetic storm, TADs originatingfrom the auroral oval may have a strong influence on the shape of the electron density profile in the F1 regionionosphere at middle latitudes. It is highly likely that TADs are responsible for the evolution of the F1 cusp

P3-079

Continuous Humidity Observation in a Tropical Region with the EquatorialAtmosphere Radar (EAR)Jun-ichi Furumoto1, Toshitaka Tsuda1, Toyoshi Shimomai2, and Toshiaki Kozu2

1. Research Institute for Sustainable Humanosphere, Kyoto University2. Interdisciplinary Faculty of Science and Engineering, Shimane University

A radar remote sensing technique that estimates humidity profiles using a wind profiler is applied to the equatorialatmosphere radar (EAR) to monitor detailed humidity variations in tropical regions. Turbulence echo powerintensity is related to the vertical refractive index gradient squared (M2). M is primarily determined by the verticalgradient of specific humidity in the lower troposphere. These relations are employed to estimate a humidityprofile. The EAR observations were carried out in November 2002. Turbulence echoes from one vertical and four obliquebeams were obtained with time and height resolution of 3 minutes and 150 m, respectively. The humidity profileswere estimated using the EAR at heights of 1.5-7.5 km. In this analysis, time-interpolated temperature profiles ofradiosonde observations were also used to estimate humidity profiles. Detailed variations of humiditycorresponded well to rain distribution observed simultaneously with the L-band boundary layer radar (BLR) andX-band radar and to the cloud bottom height observed with a ceilometer.

- 197 -

P3-080

Spring-autumn Asymmetry of Transequatorial Meridional Wind andEquatorial Spread F Occurrence Observed with SEALION IonosondeNetworkSusumu Saito and Takashi Maruyama

National Institute of Information and Communications Technology, Koganei, Tokyo 184-8795, Japan

With three ionosonde stations of the Southeast Asia Low Latitude Ionospheric Network (SEALION; Kototabang(0.2S, 100.3E), Indonesia, Chumphon (10.7N, 99.4E), Thailand, Chiang Mai (18.8N, 98.9E), Thailand) along themagnetic meridian, we have analyzed the ionospheric height variation associated with the prereversalenhancement (PRE). We have found that the north-south asymmetry of ionospheric height is more enhanced inautumn (September-October) than in spring (March-April). This indicates that the transequatorial meridional windis more stronger in autumn than in spring.Strong north-south asymmetry of the ionosphere would increase the fieldline-integrated Pederson conductivity,and suppress the plasma bubble development. The spring-autumn asymmetry of transequatorial meridional windcould be one of the important factors that result in the spring-autumn asymmetry of equatorial spread F occurrencethat have been found by previous studies.

P3-082

Propagation and Vertical Structure of Madden-Julian Oscillation overIndonesia, Especially during the First CPEA Campaign in 2004Eddy Hermawan and Nunun Nurhayati

1. National Institute of Aeronautics and Space (LAPAN), Jl. Dr. Djundjunan 133, Bandung 40173, Indonesia2. Geophysics and Meteorology Department of Bogor Agriculture University (IPB), Bogor, Indonesia

The Madden-Julian Oscillation (MJO) is the dominant mode of tropical variability (Madden and Julian, 1971,1972). It is manifested on timescales of ~30-70 days through large-scale circulation anomalies which occur inconjunction with eastward propagating convective anomalies over the eastern hemisphere. The baroclinic natureof the MJO has been eluciaded (e.g. Madden and Julian, 1971, Knutson and Weickmann, 1987). However, studieshave typically been limited to examination of one upper-tropospheric and one lower-tropospheric level, and theinterrelationships as a function of altitude have not been explored in detail. Furthermore, little attention has beendevoted to the conditions occuring during the onset of MJO convection in the western Indian Ocean. The purposeof this paper is to examine in detail the propagation and vertical structure of the MJO during the first CouplingProcesses Equatorial Atmosphere (CPEA) Campaign in 2004 and to provide a comprehensive picture of the MJOwithin the dynamically consistent framework of the NCEP/NCAR Re-analysis. This result indicates that accuraterepresentation of the moist thermodynamic processes in the boundary layer and interaction between shallow anddeep convection may be the key for describe the propagation and vertical structure of MJO over Kototabang andsurrounded area.

Keywords : CPEA Campaign, OLR, EAR, and MJO

- 198 -

P3-083

Comparison of Electron Energy Budget in the Polar Ionosphere betweenQuiet and Disturbed ConditionsYoshiko Koizumi-Kurihara1, Wlodek Kofman2, Satonori Nozawa1, and Ryoichi Fujii1

1. Solar-Terrestrial Environment Laboratory, Nagoya University2. Laboratoire de Planetologie de Grenoble

The electron fluxes precipitating at the top of the high latitude ionosphere contribute to the production ofionization, to the excitation of atmospheric constituents, and to the heating of the ambient electrons directly or bythe secondary electrons. The initial precipitated electrons lose their energy by ionization creating the secondaryelectrons, by heating of the ambient electrons and neutrals until they are assimilated into the ambient electrons.The heated ambient electrons lose this energy to the neutral gas and ambient ions. Finally, the temperaturegradient produced in the ionospheric plasma induces a heat flux. The budget equation determines the balancebetween the heating rate, the cooling rate, and the heat conduction for stationary conditions.We have studied the energy budget of ionospheric electrons by EISCAT radar data during quiet time and theHalloween Storm of October/November 2003. The intensity of the cooling rate and the heat conduction isquantitatively computed at each altitude in the ionosphere. We discuss the electron energy budget and comparequiet and disturbed conditions about energy gain and loss due to electron heat conduction.

P3-084

Preliminary Report of Electric Field Measurements in the Ionosphere byS-310-37 and S-520-23 Sounding RocketsKeigo Ishisaka1, Yuki Ashihara1, Taketoshi Miyake1, Toshimi Okada1, Yasumasa Kasaba2, Takumi Abe3, and Takayuki Ono2

1. Toyama Prefectural University, Imizu, Toyama 939-0398, JAPAN2. Tohoku University, Sendai, Miyagi 980-8578, JAPAN3. Institute of Space and Aeronautical Science (ISAS/JAXA), Sagamihara, Kanagawa 229-8510, JAPAN

S-310-37 and S-520-23 sounding rocket experiments are carried out at Uchinoura Space Center (USC) in 2007.The purpose of S-310-37 rocket experiment is an integrated observation of the high electron temperature layer inthe Sq current focus during the winter daytime over USC. In order to measure the field-aligned electric field dueto the Sq current, we develop the three-dimensional electric field detector (EFD). The EFD measures threecomponents of electric field by using 3 pair of probe antenna. On the other hand, the purpose of S-520-23 rocketexperiment is the investigation of the process of momentum transportation between the atmospheres and theplasma in the thermosphere during the summer evening time at mid latitudes. The Electric filed and VLF/MFband Receiver (EVMR) is loaded on this sounding rocket. The EVMR measures the two components of electricfield by using 2 pair of probe antenna in order to obtain a dynamics of plasma particle in the ionosphere. As a common measurement, these experiments measure the intensities and the Doppler shift of radio wave fromNHK Kumamoto broadcasting station (873 kHz, 500 kW) and JJY signal from Haganeyama LF radio station (60kHz, 50 kW). The electron density profile and the collision frequency in the ionosphere are estimated by thepropagation characteristics and the full wave method.In presentation, we will show the preliminary report of electric field and propagation characteristic of LF/MFradio waves measured by two sounding rocket experiments.

- 199 -

P3-085

Meteor Radar Observations of Short-term Tidal Variablities in theLow-latitude MLT Region: Implication of Non-linear Wave-waveInteractionsKaranam Kishore Kumar and Maria Antonita

Space Physics Laboratory, Vikram sarabhai space center, Thiruvananthapuram-695022, India.

The atmospheric tides, which are the synonym for mesosphere and lower thermosphere (MLT) dynamics, play avital role in understanding the dynamics and energetics of the Earth's middle and upper atmosphere. In the earlierphase of MLT region studies, the height profiles of tidal amplitudes and phases were treated extensively and in thelater phase the possible forcing mechanisms for the tides. From the last two decade, the interest is shifted towardsthe tidal variability at different scales. Till date, long term and seasonal variations were reported by manyresearchers. In recent years, variation of tidal amplitudes at planetary wave scales assumed importance in the fieldof middle atmospheric dynamics. In this regard, short-term variablities in the Mesosphere-Lower Thermosphere(MLT) tidal activity using meteor radar observations over Trivandrum (8.5 N, 77 E) are studied. Day-to-daydiurnal, semidiurnal and terdiurnal tidal amplitudes are estimated using continuous hourly zonal and meridionalwind measurements in the MLT region during the period of February 2006 to May 2007 over this latitude. It isobserved that tidal amplitudes do show variations shorter than the seasonal time scales. Time series data ofdiurnal, semidiurnal and terdiurnal amplitudes are obtained and the same is subjected to the wavelet analysis,which reveled the tidal variability at various time scales. The variability of tides at planetary wave scales providedenough evidence for wave-wave interaction. Further, bispectrum analysis is carried out to examine the non-linearinteractions between the planetary waves and tides. The present results also showed the seasonal dependency ofmodulation of tides by the planetary scale waves, which can be directly attributed to the variability in the sourceof both tides and planetary waves. The results of present investigations, thus, bought out the salient features ofwave-wave interactions in the MLT region over this latitude.

P3-086

Atmosphere-ionosphere Coupling over the Dip Equator: Results from theCAWSES India CampaignTarun Kumar Pant, C.Vineeth, K. Kishore Kumar, Smitha Thampi, V. Sreeja, G. Manju, Sudha Ravindran, Geeta Ramkumar, C.V.Devasia , and R.Sridharan

Space Physics Laboratory, Vikram Sarabhai Space Centre, Trivandrum, India 695022

To investigate the MLTI coupling and temporal variability of Equatorial Spread-F (ESF) in context of the Climateand Weather of the Sun Earth System (CAWSES), an international program, multi-instrumented campaign wasconducted during March-April 2006 in India. A Multiwavelength dayglow Photometer (MWDPM) was operatedalong with ionosonde, magnetometer and a meteor radar from Trivandrum (8.5 N, 76.5 E, 0.5 N diplat.), the dipequatorial station in India. The MWDPM provided the optically estimated daytime mesopause temperature whilethe meteor radar measured the wind and temperature in the lower ionospheric region. The MWDPM also providedthe near simultaneous measurements on the thermospheric dayglow (O1D 630 nm). Some new and importantobservations made during this campaign are the following:(a) The optically measured daytime mesopause temperature shows a prominent decrease in the afternoon hoursduring the main phases of the geomagnetic storms. This observation, perhaps, is new and unique.(b) Quasi 2 and 5 day oscillations appear to be modulating the mesopause temperature, wind and the EquatorialElectrojet (EEJ) induced magnetic field on the ground indicating the presence of planetary waves therein.(c) However, the simultaneously measured thermospheric dayglow (O1D 630 nm) shows an intensification of aquasi 2- and 5- day wave activity observed in equatorial Lower Thermosphere Ionosphere (LTI) region only afterMarch 18, 2006 which happens to be the day of the onset of a moderate geomagnetic storm.These measurements, as presented here, are new and will be discussed in context of the vertical coupling of theequatorial MLTI region.

- 200 -

P3-087

Reconstruction of Electron Energy Distribution by the GeneralizedComputed Aurora TomographyYoshimasa Tanaka1, Takehiko Aso2, Akira Kadokura2, and Yasunobu Ogawa2

1. Transdisciplinary Research Integration Center, Research Organization of Information and Systems, 9-10, Kaga1-chome,Itabashi-ku, Tokyo 173-8515, Japan2. National Institute of Polar Research, 9-10, Kaga 1-chome,Itabashi-ku, Tokyo 173-8515, Japan

We have studied the aurora computed tomography, which is the method to reconstruct three-dimensional (3-D)structure of auroral luminosity from multiple auroral monochromatic images simultaneously obtained by thenetwork observation, in cooperation with the Swedish Institute of Space Physics. This method is extended to theGeneralized Computed Aurora Tomography (G-CAT), by which energy distribution of auroral precipitatingelectrons is estimated from multimodal data, not only the auroral images but also electron density enhancementfrom the EISCAT radar and cosmic noise absorption (CNA) from imaging riometer.In this study, the reconstruction of electron energy distribution with the G-CAT is tested by using the modelaurora. The forward problem is based on the range calculation of the precipitating electrons. Assuming the energydistribution of the incident electrons, height profiles of auroral emission and electron density enhancement arecalculated. The observational data by the CCD cameras, the EISCAT radar, and the imaging riometer are obtainedfrom these auroral emission and electron density profiles. Then, we attempt to retrieve the energy distribution ofthe precipitating electrons from the simulated observational data. The inversion analysis is based on the Bayesianinference, in which the problem is formulated as the maximization problem of posterior probability.

P3-089

Fundamental Unresolved Problems on the Vertical Wavenumber Spectra ofInternal Atmospheric Gravity WavesT. K. Ramkumar, K. Niranjan Kumar, and D. Narayana Rao

National Atmospheric Research Laboratory, PB NO:123, Tirupati-517502, India

Detailed analyses on vertical wavenumber spectra (log-log spectrum) of lower atmospheric wind (3-22 km) andmiddle atmospheric (25-70 km) temperature perturbations measured respectively by MST radar and Nd-YagRayleigh backscattering lidar, collocated at Gadanki, India have shown spectral slope values in the range of ~ -1.7- -3.5. The same has been reported many times elsewhere using different measurement techniques. The importantquestion regarding these spectral slope values is why they are varying so much against the expected theoreticalvalue of -3. Active modeling efforts are continuing still for more than a decade to adequately explain thediscrepancy between the expected and observed slope values. To address this issue in the line of finding whethermathematical artifacts play a role, we analyzed millions of random number sets with different lengths of FFTpoints such as 64, 128, 256, 512, 1024 points etc. and calculated spectral slopes of log-log spectra as we did forthe observed winds and temperature. From the analyses of random number sets, it is found the same range ofspectral slopes as for the atmospheric parameters observations, indicating that there is something fundamentallywrong in the Fast Fourier Transform analyses methods, which produces these range of spectral slope values asmathematical artifacts. Coincidentally these values happened to be near the expected theoretical value of -3 in thestudy of internal atmospheric gravity waves. Unless the problem of mathematical artifacts is solved, it is difficultto parameterize the effects of dissipating atmospheric gravity waves in general circulation models.

- 201 -

P3-090

Indian MST Radar Observations of High Frequency and Inertia-GravityWaves from Strong Shearing Winds near the Tropopause RegionK. Niranjan Kumar, T. K. Ramkumar, and D. Narayana Rao

National Atmospheric Research Laboratory, PB No: 123, S. V. University, Tirupati-517502, India

The Indian MST radar, located at the Indian tropical station of Gadanki, has been operated often continuously forseveral hours on some days and regularly four times a day (six hours interval) for few years. The objectives of theexperiments conducted are to determine the generation mechanisms and propagation characteristics and to locatethe sources (with respect to height over Gadanki) of high frequency (periodicity of few minutes to few tens ofminutes) as well as the low frequency (periodicity of few hours) and inertia-gravity waves. As the inertial periodat the Gadanki location is ~ 51 hours, regular observation of lower atmospheric winds (~3-20 km) with six hourinterval for several years has given a good opportunity to study in detail the characteristics of inertia gravitywaves over this region particularly during the Indian south west monsoon period of June-September. Using loweratmospheric winds (3-20 km) measured with the Indian MST radar, we report in the present paper that it isobserved the generation of high frequency as well as inertia-gravity waves from strong vertically shearinghorizontal winds (Tropical Easterly Jet, TEJ) near the tropopause region particularly during the monsoon period. Itis believed that while the high frequency gravity waves are generated because of Kelvin Helmholtz instabilityprevailing in a narrow height region of within ~0.5 km, the inertia-gravity waves are generated within fewkilometers inside the TEJ located at ~ 14-17 km because of the geostropical adjustment of TEJ.

P3-091

Modeling of Solar Flare Induced D Region Perturbation in the Ionosphereand Comparison with VLF Amplitude ObservationYasuyuki T. Tanaka1, Toshio Terasawa2, Masashi Hayakawa3, Mari Yoshida3, Takumi Horie3, and Takashi Minoshima1

1. University of Tokyo, Tokyo, Japan2. Tokyo Institute of Technology, Tokyo, Japan3. University of Electro-Communications, Tokyo, Japan

High-energy photons (X-rays and gamma-rays) from solar flares produce enhanced ionization of the lowerionosphere (40 to 90 km altitude). It is known that this ionospheric disturbance is observed as unusually largeamplitude change of very low frequency (VLF) signals propagating in the Earth-ionosphere waveguide. There area lot of papers which discuss the general effects of solar flares on the D region of ionosphere. However, fewpapers concentrate on a quantitative study of the relationship between the X-ray flux of the flare and itscorresponding change in electron number density in the D region. We focus on the X1.0 solar flare on 2000 June 18. This flare was detected as a large amplitude change of VLFsignals (~8 dB) for a particular path from the Japanese VLF transmitter JJI (31 degs N, 130 degs E) to Chofustation (31 degs N, 139 degs E). We develop a Monte Carlo code, and calculate the change of electron numberdensity in the lower ionosphere during the solar flare. Here, we utilize the GOES soft X-ray data to determine thespectrum. Then, we estimate the amplitude change of VLF signals using FDTD (Finite Difference Time Domain)method, and compare the simulation result with the observation.We also discuss the ionospheric disturbance caused by galactic magnetar flares on 1998 August 27 and 2004December 27, whose X-ray fluxes are several thousands times larger than those of X-class solar flares.

- 202 -

P3-092

Diurnal and Intraseasonal Variation of UTLS Vertical Wind Disturbance inEquatorial Region Correlated with Convective ActivityToshiaki Kozu1, Yasu-Masa Kodama2, Yoshiaki Shibagaki3, Toyoshi Shimomai1, Masayuki Kawashima4, and Simon Alexander5

1. Shimane University, Matsue, Shimane 690-8504 Japan2. Hirosaki University, Hirosaki, Aomori 036-8560 Japan3. Osaka Electro-Communication University, Neyagawa, Osaka 572-8530 Japan4. ILTS/Hokkaido University, Sapporo, Hokkaido 060-0819 Japan5. RISH/Kyoto University, Uji, Kyoto 611-0011 Japan

Vertical wind variations at UTLS region measured by the Equatorial Atmosphere Radar (EAR) at Kototabang,Sumatra, between 2003 and 2006 are statistically analyzed to study the characteristics of tropospheric convectiveactivity in terms of gravity wave generation. The analyses is focused on relatively short period gravity waveshaving higher elevation angle to relate the variations to convective activity close to the EAR. Correlation analysesare performed to study the relations between vertical wind variations and rainfall, rain-top height, OLR andhorizontal wind. It is shown that the wind variances have clear dirnal variation indicating that they are caused bytropospheric convection. They also show clear intraseasonal variation which appears to be also related to changein rainfall characteristics associated with MJO phase. The correlation between variances at UT (11-13 km) andLS (17-19 km) shows some seasonal variation, which may be related to the long-term change in the propagationcharactristics of gravity waves.

P3-093

The MA Dynamics and Its Effects on Distribution of Chemical Constituentsduring Winter of 2005/06Tatyana Chshyolkova, Alan Manson, and Chris Meek

Institute of Space and Atmospheric Studies, University of Saskatchewan, Saskatoon, Canada

As a part of campaign activity associated with "Atmospheric Wave Influences upon the Winter Polar Vortices(0-100 km)" project, the dynamics of the middle atmosphere (MA) is studied using MetO stratospheric fields andradar observations at mesospheric heights. The Q-diagnostic has allowed demonstration of the day-to-dayevolution of the polar vortex during the NH winter season 2005/06 with a Major Sudden Stratospheric Warming(SSW) that occurred in January of 2006. Significant differences between North American and European sectors inzonal winds as well as planetary wave (PW) spectra are demonstrated. The influence of the atmosphericdisturbances on the distribution of chemical constituents (O3, CO2, N2O, ClO) from Aura is discussed.

- 203 -

P3-094

Links between Tropopause Variations and the Boundary Layer Processesduring the Transition to Southwest Monsoon OnsetKusuma G Rao 1, Supriya Thomas 1, K Parameswaran2, D Narayana Rao3, K S Jagannath4, B V Krishnamurthy3, K Rajeev2, C Suresh Raju2, and S C Chakravarthy5

1. Atmospheric Science Programme, ISRO, Bangalore, kusuma@isro.gov.in2. Space Physics Laboratory, VSSC, Trivandrum,India3. National Atmospheric Research Laboratory, Gadanki, India4. Master Control Facility, Hassan, India5. Space Science Office, ISRO, Bangalore

One of the objectives of 'Tropical Tropopause Dynamics Experiment' under CAWSES-India programme is tounderstand the role of atmospheric boundary layer in causing dynamical and thermodynamical variations intropopause region, particularly the humidity fluctuations which hold a key role in Global Climate change studies. The comprehensive experiment started mainly with the operation of facilities at NARL, Gadanki[13.45N,78.18]in August 2004 and the aim is to address seasonal variations in Tropopause Dynamics.An attempt has been made here to understand the links between boundary layer processes and the tropopausevariations during the transition to monsoon onset. Onset of monsoon is recognized, traditionally, in rapid increasein rainfall over Kerala located in southwest peninsular coast, being substantial and persistent over a few days. Thelatest view on monsoon onset is that it has been attributed as due to interactions between surface heating andatmospheric dynamic, thermal and hydrologic processes. Therefore the monsoon onset event sets a good groundfor the study aimed at understanding the links between boundary layer and tropopause region during convectiveconditions. In the year 2006, monsoon onset was on 26 May over Kerala and progressed covered southernpeninsular region (up to 15N) by 28 May and the entire country by 24 July 2006 as reported by IndiaMeteorological Department. Emphasis in this study is on understanding tropopause variations in humidity, temperature etc., in the cloudambient region identified based on KALPANA/METEOSAT data. An attempt is made here to analyse long term high resolution measurements from GP/Radio Sondes, from anetwork of Automated weather Stations in southern peninsular region and NCEP Re-Analysis during May 1-31,2006, a period of intense convection, to study transitions in cold point tropopause temperatures, atmosphericstability etc., during the monsoon onset and their links with boundary layer transports, stability and the large scaleboundary layer convergence and near surface gradients.A striking result is the increasing trend observed in cold point tropopause temperature a few days before themonsoon onset indicating increasing warming of the atmosphere in the tropopause region. Average Cold pointtemperatures at Cochin, Gadanki, Bangalore and Trivandrum are respectively ?83.030C, -83.330C, -83.80C and?85.10C at altitudes of 17.47km, 17.81km, 16.77km, 15.69km with standard deviations 3.0 0C 1.790C, 4.490Cand 4.390C . At the surface, relative humidity, as well shows an increasing trend and touches 100% during the onset and thereon for some days; on the other hand a consistent cooling is observed with lowering of the temperatures at thesurface. Upper air GP Sonde data reveal an increasing trend in wind speed at Lower levels, and mid- troposphericrelative humidity approaching near saturation as the transition advances towards monsoon onset. While the virtualpotential temperature profiles describe a statically unstable boundary layer on almost all days between 21-30 May, Bulk Richardson number profiles show a relatively strong stable layer above the tropopause on almost all days.Mechanisms governing strong links observed in 1:1 increasing trend between Cold Point TropopauseTemperatures and the near surface humidity gradients, are being explored with NCAR/UCAR MM5, a mesoscalemodel. Also, an effort is being made to study the impact of tropopause variations on stratospheric-troposphericcoupling during convective conditions.

- 204 -

P3-095

An Observation of Coupling between the Tropical Upper Atmosphere andthe Polar AtmosphereM. Krishnaiah1 and Y. Bhavani Kumar2

1. Sri Venkateswara University, Tirupati &#8211; 517 502, India2. National Atmospheric Research Laboratory, Gadanki-517112, India

A variety of interesting phenomena in the mesopause region have been observed for the first time over the tropicalsite Gadanki (13.5 N, 79.2 E), India using a newly developed Na resonance lidar system. The features like themodulation in Na concentrations, occurrences of sporadic sodium layer and the perturbations of atmosphericgravity wave in Na layer have been seen in the vicinity of mesopause region during the past two years ofobservations, which have not been well documented over the tropical latitudes. Moreover, an interesting couplingevent such as the enhanced Na concentrations have been observed over this tropical latitude during the winterperiod of 2005, when the polar middle atmosphere undergoes warming (sudden stratospheric warming). It hasbeen reported using the Rayleigh lidar measurements over Gadanki site (Bhavani Kumar et al., 2006) that thetropical middle atmosphere temperatures under go significant cooling during the SSW periods, however theobservations of enhanced Na in the vicinity of mesopause region, during the SSW event, is an interesting and notreported elsewhere. This could be a result of coupling processes between the tropical upper atmosphere and thehigh latitude atmosphere. The paper presents the details of investigations compiled.

P3-096

Hinode, TRACE, SOHO and Ground-based Observations of a LargeQuiescent ProminenceFrantisek Farnik1, Brigitte Schmieder2, Petr Heinzel1, Ulrich Anzer3, Guillaume Molodij2, Pavel Kotrc1, and Hinode Team

1. Astronomical Institute, Academy of Sciences, Ondrejov, Czech Republic2. Observatoire de Paris-Meudon, France3. Max-Planck-Institut fur Astrophysik, Garching, Germany

A large quiescent prominence was observed by several instruments on 25 April 2007. The temporal evolution wasregistered in H-alpha by Hinode/SOT, in X-rays by Hinode/XRT and in the 195 A line by TRACE. Moreover,GBO provided calibrated H-alpha intensities. Simultaneous EUV data were also taken by the Hinode/EIS andSOHO/SUMER-CDS spectrometers. Here we have selected the SOT H-alpha image taken at 13:44:36 UT whichshows nicely the prominence fine structure as well as the central part of the prominence channel (cavity). Wecompare this image with co-temporal ones taken by XRT and TRACE and show the intensity variations alongseveral cuts parallel to the solar limb. As recently suggested by Anzer, Heinzel and Farnik (Solar Phys., in press),the dark prominence structure clearly seen in the TRACE data is due to the prominence absorption in HI, HeI andHeII Lyman continua plus the coronal emissivity blocking due to the prominence void (channel). On the otherhand, the void clearly visible in XRT images is entirely due to X-ray emissivity blocking (no prominence structureis seen in the XRT images because of the lack of absorption at X-ray wavelengths). We use these TRACE andXRT data to estimate the level of absorption and blocking. Independently, the H-alpha integrated intensitiesprovide us with an estimate of the H-alpha opacity and this is directly related to the Lyman-continua opacity asfollows from the non-LTE transfer modeling. Therefore, we have an independent check of the results obtainedfrom TRACE/XRT. Finally, we discuss the importance of this analysis for the determinations of column densities,the ionization degree of hydrogen and helium and for the energy-balance considerations.

- 205 -

P3-097

The Lower Thermospheric and Mesospheric Wind Dynamics aboveTromsoe in September 2005Satonori Nozawa1, Asgeir Brekke2, and Yasunobu Ogawa3

1. STEL, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan2. Faculty of Science, University of Tromsoe, N-9037, Tromsoe, Norway3. National Institute of Polar Research, 9-10, Kaga 1-chome,Itabashi-ku, Tokyo 173-8515, Japan

We will report characteristics of the mean wind, quasi-2 day wave, diurnal tide and semidiurnal tide derived fromlong-run data obtained by the EISCAT UHF radar at Tromsoe (69.6 deg. N) over 22 days from September 7 to 29,2005. This data set gives us a good opportunity to investigate variations of mean winds and those waves. It shouldbe pointed out that this kind of long run data is very rare. We have also analyzed the mesospheric wind data from70 to 91 km obtained by the Tromsoe MF radar co-located at the EISCAT Tromsoe site. We will discuss altitudevariations as well as temporal variations of the winds from 70 to 119 km around fall equinox in the polar lowerthermosphere and mesosphere.

P3-098

2-Dimensional FDTD Simulations of Plasma Wave Propagations in theIonosphereTaketoshi Miyake, Shujiro Yoshino, Toshimi Okada, and Keigo Ishisaka

Toyama Prefectural University, Japan

We use several methods to analyze the propagation characteristics of electromagnetic waves in the ionosphere,such as in-situ observations with sounding rockets, remote sensing observations with radar and simulationanalysis, for example Full-wave analysis and FDTD simulations. Among various simulation methods to analyzethe propagation characteristics of electromagnetic waves in the ionosphere, FDTD simulation is very useful in thecase of the ionsphere with spatial variations. We developed, therefore, a 2-dimensional FDTD simulation codewhich can treat wave propagations in magnetized plasma. Though we need to perform full particle simulations inorder to recognize accurate characteristics of waves propagating in space plasma, FDTD simulations can beperformed with much less computer resources than those necessary for full particle simulations, in memories aswell as cpu times. Since space plasma is magnetized, it is necessary to incorporate the dielectric tensor withanisotropy and dispersibility in FDTD simulation code, in order to calculate the electromagnetic field in spaceplasma. In FDTD simulations, it is essential that how to realize an effective absorbing boundary. We developedPML (Perfectory Matched Layer) absorbing boundary condition with anisotropy and dispersibility, and succeededto realize very effective absorbing boundary.We performed FDTD simulations with several-types of electron density profiles in the ionophere, ionosphericlayer model and electron cloud model and so on, then confirmed characteristics of MF wave propagations in theionosphere. According to our simulation results, we found strong diffracted electromagnetic waves which are notpropagated directly. These diffracted waves cannot be demonstrated in Full-wave analysis with one-dimensionallayers. In this study, we compared simulation results and the in-situ observation results with S-310-33 soundingrocket launched from Uchinoura Space Center.

- 206 -

P3-099

A Study of Electron Density Disturbances Observed with Fixed BiasedProbe on S-310-37 Sounding RocketNaomi Murakami1, Takumi Abe2, and Akinori Saito1

1. Graduate School of Science , Kyoto University, Kyoto,606-8502, Japan2. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, 229-8510, Japan

The sounding rocket S-310-37 was launched from Uchinoura (31.15N, 131.05E) to study the Sq focus region, at11:20:00 JST on 16 January 2007. The purpose of this rocket experiment is to investigate the generationmechanism of the extreme increase of electron temperature around the Sq focus.According to the study from 13 rocket experiments over Japan around 11:00 JST, the electron temperatureremarkably increased between 95km and 115km of altitude with a thickness of several kilometers around the Sqfocus in winter. The electron temperature increased by 200-1000K against the background. In S-310-37 rocket experiment, the instruments on board started observation from the altitude of 67km, and therocket reached the max altitude of 138km. The observed altitude profile of the electron temperature shows thelocal enhancement by 500-600K against the background around the altitude of 97-101km during the rocket'sascent. No electron temperature enhancement was seen during the rocket's descent. The FBP (Fixed Biased Probe) measured electron density disturbances. During the rocket's ascent, it observedsevere electron disturbances with high frequency up to 800Hz from 95km to 138km of altitude, which correspondsto the spatial scale of 2-10m along the rocket trajectory. The amplitude of the electron density disturbances duringthe rocket's ascent was more than 7% of the background electron density. The spectrum power became weakerduring the rocket's descent.In this presentation, we will show the analysis of FBP data in detail and discuss the mechanism of electron densitydisturbances around the Sq focus.

P3-100

Characteristics of Sporadic Na layers in the Mesopause Region overIndonesia Observed by LidarChikao Nagasawa1, Makoto Abo1, Yasukuni Shibata1, and Takuji Nakamura2

1. Faculty of System Design, Tokyo Metropolitan University, Hino, Tokyo 191-0065, Japan2. Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Kyoto 611-0011, Japan

Characteristics of metallic layers in the mesopause region over the equator observed with the resonance scatteringlidars installed at Kototabang, Indonesia (0.2S, 100.3E) are reported. The sporadic sodium layer (Nas) were oftenobserved during the intensive observation from July to August, 2005. Nas layers appeared above 90 km. In themid-latitude, the correlation of Nas with the strong wind shear is reported at Shigaraki, Japan (35N). But, atKototabang, many Nas events are observed with the wind shear weaker than the mean wind shear. Especially, Naswith the bad correlation with wind shear is generated at dawn (2&#8211;4 h LT), and Nas with the goodcorrelation with wind shear is mainly generated before midnight.

- 207 -

P3-102

Atmospheric Tides in the Mesosphere/Lower Thermosphere over theEquator by Radar ObservationsTakuji Nakamura1, Toshitaka Tsuda1, Sundararajan Sridharan2, and Robert A. Vincent3

1. Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Kyoto 611-0011, Japan2. National Atmospheric Research Laboratory, Tirupati-517 502 India3. Faculty of Sciences, University of Adelaide, Adelaide SA, 5005 Australia4. Master Control Facility, Hassan, India

In the Japanense CPEA (Coupling Processes in the Equatorial Atmosphere) project, we haveinstalled/re-arranged three radars for observing dynamics of the mesosphere and lower thermosphere; a meteorradar in Kototabang (0S, 100E, started continuous observation in Nov. 2002), two MF radars in Pontianak (0N,109E; upgraded observation started in October 2002) and Pameungpeuk (7.5S, 107.5E, observation started inMarch 2004). The three radars in Indonesia are located over a very active convective region in the equatorialtroposphere. In this paper, characteristics of atmospheric tides in the equatorial MLT region will be discussed. Theglobal structure of diurnal and semidiurnal tides have been clarified using recent satellite observations. It is nowunderstood that besides migrating tidal components, westward propagating (wavenumber=w3), standing (we0)and eastward propagating (e3) waves have significant amplitudes. Among these, eastward propagating e3 wave isconsidered to be excited by tropospheric convections. The four year observations of Kototabang MWR showedthat diurnal oscillations in zonal wind was enhanced in October-November 2003 and November-December 2005(the latter period coincides with the CPEA-II campaign period). The phase difference between the radars atKototabang and Pontianak suggests the enhanced component was due to eastward propagating non-migrating tide.The correlation with the diurnal variation of OLR is also be discussed in the paper.

P3-104

Long-Term Trends in the Ionosphere: Overall Pattern and Open ProblemsJan Lastovicka

Institute of Atmospheric Physics, Bocni II, 14131 Prague, Czech Republic

Increasing concentration of greenhouse gases in the atmosphere affects also the ionosphere. Lastovicka et al.(Science, 314 (5803), 1253-1254, 2006) briefly presented for the first time a pattern of global change in the upperatmosphere and ionosphere. Here we focus on global change/long-term trends in the ionosphere. The lowerionosphere (below ~100 km) and the E-region and F1-region behave as expected from model estimates of theeffect of increasing concentration of greenhouse gases, mainly of carbon dioxide. Their heights are somewhatdecreasing as a consequence of thermal contraction of the upper atmosphere, the electron density at fixed heightsin the lower ionosphere is increasing due to decreasing height of the lower ionosphere, and foE and foF1 areslightly increasing as a consequence of cooling-related changes in chemistry of minor constituents. On the otherhand, there is substantial contradiction in trends in foF2 and hmF2, the results of different authors providing evenopposite signs of trends; the trend interpretation is also different, the main driver being long-term changes ofgeomagnetic activity or the greenhouse effect. Recent results show that at present the trend in hmF2 is probablydominated by the greenhouse effect, while trends in foF2 may still be dominated by geomagnetic activity, amongothers because models provide a very small greenhouse effect in foF2. The role of greenhouse gases in trendsappears to increase towards present.

- 208 -

P3-105

New Insight for Solar Influence on Geomagnetic ActivityTsutomu Nagatsuma

Applied Electromagnetic Research Center, National Institute of Information and Communications Technology, 4-2-1Nukui-kita, Koganei 184-8795 JAPAN

It is well known that geomagnetic activity shows diurnal and semiannual variations. The cause of these variationsconsists of two effects. One is the periodical change of the solar wind parameters due to a variation of thegeometrical condition between the solar wind and the Earth's magnetosphere. The other is the periodical change ofthe S-M-I coupling efficiency. The former effect has been studied in detail. However, the cause of the latter effectremains an open question. We have studied the variations for the efficiency of S-M-I coupling using the Kmindex, the F10.7 index, and solar wind data from 1965 to 1996. Our results show that the efficiency of S-M-Icoupling has diurnal, semiannual, and solar activity variations, which corresponds to the conductivity variations inthe southern and northern polar caps. The coupling efficiency during the period of high solar activity tends to belower than that during the period of low solar activity. This suggests that the solar cycle variations of geomagneticactivity are caused by the combinations of solar EUV activity and solar wind activity. High geomagnetic activityduring the declining phase of the solar cycle is caused by both the recurrent corotating interaction regioncorresponds to low latitude coronal hole and the low solar EUV activity. High solar activity depresses theefficiency of the S-M-I coupling.

P3-106

Implication of High-energy Galactic Cosmic Ray Anisotropy on the LocalInterstellar Magnetic FieldKazuoki Munakata (Tibet AS-gamma collaboration)1

1. Department of Physics, Shinshu University, Matsumoto 390-8621, Japan.2. Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan.

This paper presents the sidereal anisotropy of multi-TeV galactic cosmic ray (GCR) intensity observed by theTibet Air Shower experiment. The observed sky-map of the directional anisotropy clearly shows the large-scalefeature consisting of excess and deficit of the relative intensity. We note that the observed angular separationbetween the excess and the deficit is ~120 deg, which is much smaller than 180 deg expected from theuni-directional flow but significantly larger than 90 deg expected from the bi-directional counter streaming.According to our preliminary least-square analysis, the large-scale feature can be reproduced by a combination ofthe uni-directional and bi-directional flows with reference axes perpendicular to each other. We suggest that suchtwo streams can be expected if the GCR population is lower at the location of the heliosphere in the localinterstellar cloud (LIC) than that outside LIC. If this is the case, the orientation of the local interstellar magneticfield (LISMF) can be inferred from the reference axis of the bi-directional streaming. We discuss the orientationof the derived LISMF in comparison with those reported from other measurements of the polarization of lightfrom nearby stars, the neutral hydrogen velocity and 2-3 kHz radio emission from the outer heliosphere.

- 209 -

P3-107

Pi2 Pulsations Observed by Multiple Ground Stations and Satellites overWide Latitude: Evidence of PVR ModeM. Teramoto1, M. Nose2, and K. Takahashi3

1. Department of Geophysics, Graduate School of Science, Kyoto University2. Data Analysis Center for Geomagnetism and Space Magnetism3. Applied Physics Laboratory, Johns Hopkins University

Pi2 pulsations are defined as damping oscillations at 6.7-25 mHz, which are observed at substorm onset. On July24, 1986, we investigated Pi2 pulsations observed simultaneously by the polar orbiting DE-1 satellite (an apogee:about 3.6 Re altitude and a perigee: about 500km altitude) and equatorial orbiting AMPTE/CCE satellite (anapogee: about 8.8 Re altitude and a perigee: about 1100km altitude) in the compressional component. DE-1 andAMPTE/CCE might be located outside the plasmasphere (L=8.7) and near the plasmapause (L=3.2) at 1804-1814UT. Each of them had high coherence and the phase difference is 180 degrees. They have high coherence withthat observed at Kakioka (KAK) in the H component, which was located at L=1.25 and 3.21 MLT. The phasedifference between KAK and DE-1 and between KAK and AMPTE/CCE are 180 degrees and 0 degrees. ThesePi2 pulsations have high coherence with that observed by satellite. These observational results may support thatPi2 pulsation at low latitude are excited by the plasmaspheric virtual resonance mode, in which the ambientmagnetic fields outside plasmasphere oscillated with the cavity mode resonance because the plasmapause wasimperfect boundary. We will also conduct statistical study of Pi2 pulsations, which were simultaneously observedby the DE-1 and AMPTE/CCE satellite.

P3-108

Seasonal Variation of MeV Electron Flux at Geostationary OrbitTakahiro Obara

NICT, 4-2-1, Nukuikita, Koganei, Tokyo 184-8795, Japan

Recent detailed observations of the storm-time dynamics of the outer belt electrons revealed the dependence ofrebuilding location of the outer radiation belt on the magnitude of the storms ; i.e. the location of the newlyappeared outer belt is inversely proportional to the storm bigness. An interesting observation is the simultaneousappearance of intense whistler mode chorus emissions around the peak position of electron flux.Puzzling aspect of the increase of relativistic electrons is the increase of relativistic electrons around thegeostationary orbit during non-storm-time period. The increase of energetic electrons has close relationship withthe plasma wave activity. Supply of intermediate-energy electrons is evident, corresponding to the substorminjections. These seed electrons are likely accelerated by the waves to the relativistic energy range. Well knownphenomena of the increase of the relativistic electron flux around the geostationary orbit is the dependence on thesolar wind velocity. We have newly found that increase of the relativistic electron flux strongly depends on theIMF polarity. During the away polarity the electron flux increases very much in the autumn season, and during thetoward polarity the electron flux increases very much in the spring season. Our observations are largely consistentwith so-called Russell-McPheron effect, in which the substorm activity depends on the IMF polarity especially inspring and autumn seasons. We will compare the energetic electron data at geostationary orbit with the data frompolar orbiting satellite to consider outer radiation belt dynamics from the magnetic activity point of view.

- 210 -

P3-109

Long-term Change in Geomagnetic Activity at Syowa Station in Antarcticaand Kakioka ObservatoryAkio Yoshida and Akira Kadokura

National Institute of Polar Reseach, Kaga 1-9-10, Itabashi, Tokyo 173-8515, Japan

On the basis of the K-index data at Syowa Station and the Kakioka observatory since 1966, we investigatedlong-term changes in the geomagnetic activity. The geomagnetic activity at Syowa Station as well as Kakiokaincreased before 1990 and declined after that which coincides with the long-term change in the geomagneticactivity derived from the data of the aa-index (Clilverd et al., 1998). Our new finding is that the ratio of thegeomagnetic activity at Syowa Station relative to that at Kakioka has been continuing to increase after 1990. Thecause of the increase of the ratio can not be attributed to changes in solar activity or rises in the averageinterplanetary magnetic field strength, for the ratio has been increasing after the geomagnetic activity started todecline. It is noteworthy that the number of the K-index smaller than 2 at Syowa Station has been decreasing andthe decrease is clearer for months of the summer season in Antarctica. We think the increase of the geomagneticactivity relative to that at Kakioka may represent change in the conductivity or the height of the ionosphere due tocooling of the upper atmosphere that was caused by the increased concentration of greenhouse gases. Although ithas been estimated that the change in the height of the E-layer is not so large (Rishbeth, 1990), we suppose thatthe effect of the cooling may appear in an enhanced scale in the Antarctic region.

P3-110

On-Line Geomagnetic Database for Space Climatology: Progress Report inCAWSESToshihiko Iyemori1, Masahito Nose1, Masahiko Takeda1, Yoko Odagi1, Juergen Matzka2, Sobhana Alex3, and Evgeny P. Kharin4

1. Graduate School of Science, Kyoto University, Kyoto 606-8502, Japan2. Danish Meteorological Institute, Lyngbyvej 100, DK-2100, Copenhagen, Denmark3. Indian Institute of Geomagnetism, Colaba, Mumbai 400 005. India4. WDC for Solar-Terrestrial Physics, Molodezhnaya 3, Moscow, 117296, Russia

Modern geomagnetic observation started in the middle of the 19th century and has produced a huge amount ofmagnetograms which record geomagnetic variations on photographic paper. Since geomagnetic disturbances areclosely relate to the solar activity, in particular to solar wind parameters, a long series of geomagnetic data canalso give us independent information on long-term variations in the solar activity, which the sun spot numbercannot indicate. Therefore old geomagnetic data could be useful also in investigating climate change. Taking intoaccount the change of user requests, i.e., from analog paper copy to digital file, and the importance of oldgeomagnetic records, we have been trying to digitize the hourly tables or microfilmed magnetograms. In the lastseveral years, we have been constructing digital image files from microfilmed magnetograms or from originalmagnetograms at observatories, and they are available at our web site page(http://wdc.kugi.kyoto-u.ac.jp/film/index.html). Here we report our recent progress in geomagnetic databaseconstruction for the study of space climatology.

- 211 -

Author Index Bold designates the presenter. Abe, S., SB32-1, SB51I-2, P3-047 Abe, T., SA32-2, P3-084, P3-099 Ables, S. T., SB51-3 Abo, M., P3-077, P3-100 Adachi, T., SA12-1, SA31-3 Afroz, R., P1-109 Agarwal, K., P1-010 Aggarwal, M., P1-023 Ahmad, N., P1-039 Akiyama, S., SA11-1, P1-092 Akiyoshi, H., SA21-5 Alex, S., P1-032, P1-045, P3-110 Alexander, S. P., SA51-4, P1-105, P3-069, P3-092 Ali, M. A. M., P1-007 Aliyeva, S., P1-086 Alperovich, L., P1-090 Alyana, R., P3-018 Amano, M., SB21-5, SB42-6 Amano, T., P1-077 Amata, E., P3-059 Ambroz, P., P1-008 Anastasiadis, A., P3-019 Anderson, R. R., P1-028 Andre, M., P3-032 Angelopoulos, V., SB51-1 Antolin, P., P1-054 Antonita, M., P3-063, P3-085 Antonita, T. M., P3-061 Anzer, U., P3-096 Aoki, Y., SA31-3 Aoyama, T., P3-026 Araki, T., P1-044 Aran, A., SB52-2 Asai, A, SB12I-2, SB12-3, P1-072 Asai, K., P1-056 Asamura, K., SB41-2, P1-027, P3-041 Asano, E., SB42I-1, SB42-4, P3-035 Asgarov, A. B., P3-023 Ashihara, Y., P3-084 Aso, Takehiko, SA52-4, P3-087 Aso, Teruo, P1-056 Astafyeva, E. I., P1-096 Austin, J., SA21I-2 Avakyan, S. V., SA11-4 Babayev, E. S., P3-023, P1-026, P1-086 Bailey, S. M., SA12Ｉ-1, SA41I-5

Balasis, G., P3-019 Baldwin, M., SA52Ｉ-2 Balikhin, M. A., P1-070, P3-032 Bando, T., SB12-5, SB21I-1 Banola, S., P1-029, P3-074 Bargatze, L. F., SB22-6 Batista, P. P., P3-072 Baumjohann, W., P3-019 Becker, E., SA41I-1 Beer, J., K1-1 Beig, G., P1-101 Beranova, R., SA22-6 Berger, T. E., SB11-2, SB12I-1, SB21I-2 Bewsher, D., SB21-1 Bhardwaj, S. K., P1-014 Bharti, L., P1-111 Bhattacharya, S., P1-036 Bhattacharyya, A., P3-062 Billings, S. A., P1-070 Bisi, M., SB21-1, P1-062 Bisi, M. M., SA11I-2, P1-055 Bittner, M., SA32-3 Bochnicek, J., SA22-6 Bondo, T., SA12Ｉ-2 Bottollier-Depois, J. F., P3-051 Brahmanandam, P., P1-068 Brandt, P. C., P3-043 Brasseur, G. P., SA32I-1 Breen, A., SB21-1 Breen, A. R., P1-055 Brekke, A., P1-059, P3-097 Bruinsma, S. L., SA31-1 Bryukhanov, V. V., P1-037 Buchert, S. C., P1-078 Buffington, A., SA11I-2, P1-055 Buresova, D., P1-052 Buriti, R. A., P3-072 Bychkov, V. V., P3-039 Cabello, I., P1-017 Cappallo, R. J., P1-071 Carlson, C. W., P1-073, P3-030 Carlsson, M., SB12I-3 CAWSES Tidal Campaign Team, SA31I-2 Cebula, R. P., SA21-1 Cerrato, Y., SB52-2 Chakrabarty, D. D. K., P1-098 Chakravarthy, S. C., P3-094 Chakravarty, S. C., SA11-5 Chandra, H., P3-074 Chang, T. F., SB32-4

Chao, C.-K., P3-003 Chashei, I. V., SB22-5 Chen, A. B.-C., SA12-1 Cheng, C. Z., SB32-4, P1-019 Chi, P. J., SB51I-1, SB51-1 Chifor, C., SB12I-2 Cho, K.-S., SB21-2, P1-089, P1-97 Cho, Y.-M., SA32-3, SA32-4 Choi, H.-J., SA51I-1 Chshyolkova, T., P3-093 Chun, H.-Y., SA51I-1, SA51-3, P1-020 Cid, C., SB52-2 Cifuentes-Nava, G., P1-041 Clemesha, B. R., P3-072 Clover, J. M., P1-055 Coca, D., P1-070 Coco, I., P3-059 Collins, R. L., SA51-1 Coster, A., SB12-2 Cremades, H., SB52-2 Crothers, S., SB21-1 Cubasch, U., SA52-1 da Silva, M. R., P1-030 Daglis, I. A., SB31-3, P3-019, P3-049 Das, I. M. L., P1-107 DasGupta, A., P1-050 Dasso, S., SB52-2 Davis, C., SB21-1 Davis, J., SB21-1 de Lucas, A., P1-030 Deepa,V., P3-061 DeLand, M. T., SA21-1 Delcourt, D. C., P3-049 DeLuca, E. E., SB11-1, SB12-1, SB12-5, SB21I-1 Deng, X., P3-078 Dergachev, V., P1-022 Deushi, M., SA21-3, SA22-3 Devasia, C. V., P1-034, P1-061, P1-093, P3-055, P3-074,

P3-075, P3-086 Dhaka, S., SA51-3 Dhaka, S. K., P1-020 Dhar, A., P3-033 Dikpati, M., K3-3 Dimitrova, S., P1-026, P1-086 Djamaluddin, T., P3-009 Dmitrova, S., P3-023 Dolenko, S. A., P3-002 Domingo, V., P1-017 Donovan, E., P3-041 Donovan, E. F., P1-028

Dorrian, G., SB21-1 Dorrian, G. D., P1-055 Dryer, M., SB41-1 Dunlop, M., P3-032 Dutta, G., P1-105, P3-101 Dwivedi, V., P1-024 Ebihara, Y., SB41-2, P1-058, P3-041, P3-043 Echer, E., SB52-1 Echer, E., P1-002, P1-030 Ejiri, M., SA52-4 Ejiri, M. K., SA42Ｉ-4 Electric Field and Plasma Wave Investigation Team, P3-038 Ella, E. M. A. E., P1-051 Emmert, J. T., SB52Ｉ-1 Emperumal, K., P3-071 Engebretson, M., P3-037 Engebretson, M. J., SB32-5, SB51I-1 Erickson, P. J., P3-050 Eselevich, M., P1-112 Eselevich, V., P1-112 Evangelista, H., P1-002 Eyles, C., SB21-1 Eyles, C. J., SB21-6 Fallows, R., SB21-1 Fallows, R. A., P1-055 Farnik, F., P3-096 Fedorov, E., P1-090 Fedorov, E. N., P1-088 Ferriz-Mas, A., P1-113 Feynman, J., SA12-5 Fiore, B. D., P3-019 Fok, M.-C., SB31-3, P3-043, P3-049 Forbes, J. M., K4-3, SA31-1, P1-048 Forbes, T. G., SB41Ｉ-1 Foster, J. C., P3-050 Fraser, B. J., SB51-1, SB51-2, P3-052 Fraser, G. J., P1-007 Frey, H. U., SA12-1, P3-041 Fritts, D., SA42Ｉ-1 Frohlich, C., K5-3 Fry, C. D., SB41-1 Fujii, R., SA31-2, SA32-2, P1-067, P1-078, P1-082, P3-083,

P1-100 Fujiki, K., SB21-4, SB22-1, P1-047, P1-112 Fujimoto, M., P1-063 Fujita, S., SB32-6, SB42-5 Fujiwara, H., SA32I-2, SB32-6, SA41I-2, P3-070 Fukao, S., K3-4, SA51-3, P3-060, P3-064 Fukazawa, K., SB32-6, P3-026 Fukunishi, H., SA12-1

Fuller, N., P3-051 Fung, S. F., SB31I-3 Furumoto, J., P3-079 Furuya, N., P3-034 Fushishita, A., P3-036 Ganji, Y., P1-003 Ganushkina, N. Y., P3-025 Garcia, R. R., SA22-4, SA42-1, SA52I-1 Gary, P. Z., SA11-2 Geller, M. A., Ｔ3 Georgieva, K., P1-026, P1-086 Georgiou, M., SB31-3, P3-019 Geranios, A., SB22-2 Ghosh, S. S., P3-021 Giorgetta, M. A., SA32I-1 Goldstein, J., P3-052 Gonzalez, A. L. C., SB52-1 Gonzalez, W. D., SB52-1, P1-030 Gonzalez-Esparza, A., P1-041 Gopalswamy, N., K2-2, SA11-1, P1-092 Gorelenkov, N., SB32-4 Gosling, J. T., K4-1 Goto, Y., P3-038 Gray, L. J., SA21Ｉ-3 Guarnieri, F. L., P1-030 Gurubaran, S., SA32-1, P3-066, P3-071, P3-072 Gwal, A. K., P1-036 Hada, T., SB21-3, P1-079 Haefele, A., P1-065 Hagan, M. E., SA31Ｉ-1 Haigh, J. D., Ｋ2-1 Hameed, S., P1-011 Hamilton, K., SA51I-2 Han, D., P1-044 Hanchinal, A., P3-033 Handa, H., P1-082 Hanuise, C., P3-057 Hara, H., SB11Ｉ-1, SB12-3 Harra, L. K., SB11Ｉ-1 Harrison, R., SB21-1 Harrison, R. A., SB21-6 Harvey, V. L., SA12Ｉ-1 Hashiguchi, H., SA51-3, P1-013, P3-060, P3-064 Hashimoto, K. K., SB32-2 Hayakawa, H., P1-083 Hayakawa, M., P1-090, P3-091 Hayashi, K., P3-004 He, H., P3-053 Heinzel, P., P3-096 Hejda, P., SA22-6

Hermawan, E., P3-082 Hernandez-Quintero, E., P1-041 Hick, P., P1-062 Hick, P. P., SA11I-2, P1-055 Higuchi, T., P3-043 Hinode J team, SB11-6 Hinode Japan/US SOT team, SB11-4 Hinode SOT/XRT Team, SB12-4 Hinode Team, P3-096 Hinode U team, SB11-6 Hinode/SOT team, P3-012 Hirahara, M., SB41-2, P1-027, P3-041 Hirai, M., P1-069 Hirayama, Y., P3-044, P3-046 Hirooka, T., SA21-5 Hobara, Y., P1-070, P3-032 Hocke, K., SA22-1, P1-064, P1-065 Hokkaido HF Radar Group, P1-057 Holdsworth, D. A., SA41-2, SA52-2 Hori, K., P3-029 Hori, M. E., SA21-2 Hori, T., P1-056, P1-063, P1-085 Horie, T., P3-091 Horinouchi, T., P3-060 Hoshino, M., P1-069, P1-077 Hosokawa, K., P1-057, P1-058, P1-059, P1-063, P1-085 Howard, R. A., SA11-1, SB21-6 Howard, T. A., SB21-6 Hsu, R.-R., SA12-1 Hughes, W. J., P3-040 Hui, D., P1-050 Huth, R., SA22-6 Ichimoto, K., SB11Ｉ-2, SB11-1, SB11-2, SB11-3, SB11-4,

SB12I-1, SB12-4, SB21I-2, P1-114 Ieda, A., SB32-3, P1-083 Iida, Y., P1-012 Iijima, M., P3-038 Iizima, M., SB31I-2, P1-074, P3-016 Ikeda, A., P1-035, P1-076, P3-039, P3-044 Imachi, T., P3-038 Imada, S., SB12-3 Inoue, S., SB11Ｉ-2, SB11-5, SB42I-1, P3-012 Ishii, K., P3-076 Ishii, M., P1-110, P3-070 Ishii, T. T., P1-046, P1-060 Ishikawa, R., SB11-3 Ishisaka, K., P3-038, P3-084, P3-098 Ishitsuka, J. K., SB51-3 Ishitsuka, M., SB51-3 Islam, M. N., P1-109

Isobe, H., SB11-3, SB12I-2 Ito, H., SB21-4 Ito, K., SA21-4 Ito, M., P1-035 Itoh, H., SB22-1 Iwagami, N., SA32-2 Iyemori, T., P3-110 Iyer, K. N., P1-023, P1-053, P3-065 Jaaffrey, S., P1-111 Jackel, B., P3-041 Jackman, C. H., SA12Ｉ-1 Jackson, B., P1-062 Jackson, B. V., SA11I-2, SB21-6, P1-055 Jacobi, C., SA32-3 Jadav, R. M., P1-053 Jadeja, A. K., P1-053 Jagannath, K. S., P3-094 Jain, A. R., P1-020 Jain, R., SB12I-2 Jaiswal, R. S., P1-106 Jarvis, M. J., SB52Ｉ-1 Jee, G. H., SA52-3 Jensen, E. A., SA11I-2, P1-062 Jiang, J. H., SA32-3 Jibben, P. R., SB12-1, SB21I-1 Jin, H., SB32-6, P3-070 Johnston, J. C., SB21-6 Jordanova, V. K., P3-013 Joshi, C., P1-111 Joshi, H. P., P1-023, P1-053, P3-065 Joy, S. P., SB52I-2 Kadokura, A., P1-074, P3-087, P3-109 Kaempfer, N., SA22-1, P1-064 Kageyama, A., P3-028 Kakad, A. P., P1-038 Kakad, B., P3-062 Kamide, Y., K3-1, SB32-3, P1-056, P1-063 Kamio, S., SB12-3 Kamobe, M., SB51-4 Kampfer, N., P1-065 Kano, R., SB11-1, SB12-1, SB12-5, SB21I-1 Kapiris, P., P3-019 Kartalev, M., P3-059 Kasaba, Y., SB41-2, P1-027, P1-035, P3-038, P3-041, P3-084 Kasahara, Y., P3-038 Kasper, J. C., P1-071 Kataoka, R., SB31I-1, SB42I-1, P1-056, P1-057, P1-058,

P3-006 Katoda, M., SB51-4 Katoh, Y., SB31-1

Katsukawa, Y., SB11Ｉ-2, SB11-1, SB11-2, SB11-3, SB11-4, SB12I-1, SB12-4, SB21I-2, P1-114

Kaushik, S. C., P1-010 Kawahara, T. D., SA41I-3 Kawamura, M., P1-110 Kawano, H., SB32-1 Kawashima, M., P3-092 Kawatani, Y., SA42I-2, SA42I-5, SA51-2 Kawate, T., SB11-6, P1-114 Keckhut, P., P1-065 Keika, K., P3-043 Keller, M., SA32I-1 Keremidarska, V., P3-059 Khabarova, O., P3-056 Khabarova, O. V., P3-023 Kharin, E. P., P3-110 Kiatai, R., SB11-6 Kikuchi, T., SB32-2, P3-011, P3-017, P1-040, P1-056, P1-057,

P1-058, P1-085 Kim, H.-J., P3-008 Kim, J.-H., SA52-3 Kim, K.-H., P1-066 Kim, K.-S., P1-097 Kim, R.-S., P1-089 Kim, S. W., P1-089 Kim, Y. H., SA52-3, SB41-5 Kimura, G., SB51-3, SB51-4, P1-060 King, T. A., SB52I-2 Kitagawa, H., SA21I-1 Kitai, R., SB51-3, SB51-4, P1-046, P1-060, P1-114 Kitamura, K., P1-056, P3-047 Kitamura, M., SA21-5 Kitamura, N., P3-016 Kitazawa, K., SA21I-1 Klimenko, M. V., P1-037 Klimenko, V. V., P1-037 Klimushkin, D. Y., P3-037, P3-048 Kodama, Y., P3-092 Kodera, K., SA21-2 Kofman, W., P3-083 Koizumi-Kurihara, Y., P3-083 Kojima, H., P1-091, P3-038 Kojima, M., SA11I-2, SB21-4, SB22-1, P1-047, P1-055 Kolstrom, T., P1-022 Komatsu, K., P3-015 Kombiyil, R., P1-035 Kondo, A., P3-054 Kondo, J., P3-028 Kondo, K., SB41-6 Kondoh, K., P3-005

Korreck, K., P3-040 Korotova, G. I., SB41-3 Kosovichev, A., SA11I-1 Kotoku, J., SB12-5, SB21I-1 Kotrc, P., P3-096 Kovalenko, V. A., P1-006 Kovaltsov, G. A., P1-004 Kozu, T., P3-064, P3-069, P3-079, P3-092 Kozyra, J. U., K3-2 Kozyreva, O., P1-022 Krishna, S. G., P3-014 Krishnaiah, M., P3-095 Krishnamurthy, B. V., P3-094 Krivolutsky, A., P3-067 Krucker, S., P1-019 Kubin, A., P1-016 Kubo, M., SB11-1, SB11-4, SB21I-2 Kubo, Y., SB32-6 Kubyshkina, M. V., P3-025 Kuchar, T. A., SB21-6 Kudo, K., P3-017 Kumamoto, A., SB31I-2, P1-027, P1-040, P1-074, P3-016,

P3-038 Kumar, A., P1-033 Kumar, B., P3-063 Kumar, K. K., P3-061, P3-085, P3-086 Kumar, K. N., P3-089, P3-090 Kumar, M. C. A., P1-105 Kumar, P. V., P3-101, P1-105 Kumar, S., P1-033, P3-063 Kumar, Y. B., P3-095 Kunitake, M., P1-056, P1-085 Kurihara, J., SA32-2 Kuroda, Y., SA22-3 Kurokawa, H., P1-072 Kusano, K., SB41-7, SB42I-1, SB42-1, SB42-3, P3-006,

P3-012 Kuwabara, T., P1-030 Kysely, J., SA22-6 Labitzke, K., K1-2 Lago, A. D., P1-030 Lakhina, G. S., P3-021, P1-032, P1-038 Lal, M., P1-080 Langemats, U., SA22-2, SA52-1, P1-016 Lantos, P., P3-051 Lastovicka, J., P1-052, P3-104 Latteck, R., SA41-2 Lavraud, B., P3-013 Lee, C. S., SA52-3 Lee, C.-C., P3-001

Lee, D., SB22-7 Lee, D.-Y., P3-008 Lee, J. N., P1-011 Lee, J.-Y., P1-097 Lee, K.-S., P1-097 Lee, L.-C., SA12-1 Lin, C., P3-007 Lin, J., P3-040 Lin, R. P., P1-019 Liou, K., P1-083 Lites, B., SB11-1 Lites, B. W., SB11-2, SB11-3, SB11-4, SB21I-2 Liu, C.-H., P3-003, P3-007 Liu, G., SA32-4 Liu, H., SA12Ｉ-1, SA41-1 Liu, J. -Y., P3-007 Lonsdale, C. J., P1-071 Lopatin, E., P1-022 Lotfi, B. J., SB42-2 Lu, G., SA11-3 Luebken, F.-J., K2-3 Luehr, H., P1-044 Lund, E. J., P1-073 Lund, T., SA42Ｉ-1 Lundquist, L., SB12-5 Lyons, L., SB22-7 Machida, S., P1-063, P1-083 Maeda, G., SB51I-2 Maeda, N., SB32-1 Maeda, S., P1-059 Magara, T., P3-012 Magara, T., SB11Ｉ-2 MAGDAS Group, SB51I-2, P3-044, P3-047 MAGDAS/CPMN Group, P3-046 Magnes, W., P3-019 Mandal, T. K., P1-020 Mandrini, C., SB52-2 Manik, T., P1-013 Manju, G., P1-061, P1-093, P3-055, P3-074, P3-086 Mann, I. R., SB32-5, SB51I-1, SB51-1 Manoharan, P. K., SB21-4, SB22-3, P1-053, P1-055 Manson, A., P3-093 Manzini, E., SA32I-1 Marsh, D. R., SA12Ｉ-1, SA22-4, SA41-1, SA52I-1 Marubashi, K., SB21-2 Maruyama, T., P1-110, P3-080 Mase, K., SB42-6 Mason, H. E., SB12I-2 Masuda, K., SA21I-1, SB52-4 Masuda, S., SB11-5, P1-009, P3-012

Mathew, T. J., P3-075 Matsumi, Y., SA12-4 Matsumoto, T., SB11-6, SB42I-1, SB42-4, P1-114, P3-035 Matsumoto, Y., P3-027, P3-042 Matsuoka, A., P1-027, P3-038 Matsuzaki, K., SB12-3 Matthes, K., SA22I-1, SA22-2, SA22-4 Matzka, J., P3-110 Maute, A., SA31Ｉ-1 Mazaudier, C., P1-035 Mazur, N. G., P1-088 McFadden, J. P., P1-073, P3-030 McIntosh, D., SA52-2 McIntosh, S. W., P1-049 Meek, C., P3-093 Mende, S., SB22-7 Mende, Stephen. B., SA12-1 Mende, Steven. B., P3-041 Mendoza, B., P1-001 Menietti, J. D., P1-028 Menvielle, M., SB52-2 Merka, J., SB52I-2 Merzer, M., P1-090 Metallinou, F.-A., SB31-3, P3-049 Michalek, G., SA11-1 Middleton, H., SB21-1 Mills, M., SA12Ｉ-1 Minoshima, T., P1-075, P3-091 Mironova, I. A., SA12-3 Misawa, H., P1-028 Misra, D. S., P3-018 Misran, N., P1-007 Mitchell, D. G., P3-043 Mitchell, N. J., P3-072 Mitra-Kraev, U., P1-021 Miyahara, H., SA12-1, SA21I-1, SB52-4, P1-018 Miyahara, S., SA51-2 Miyake, T., P3-084, P3-098 Miyake, Y., P1-091 Miyaoka, H., P1-074 Miyashita, Y., SB41-2, P1-063, P1-083, P1-085 Miyazaki, K., SA42I-5 Miyoshi, T., SB41-7, SB42I-1, P3-012 Miyoshi, Yasunobu, SA41I-2, SA32I-2, SB32-6, P3-070 Miyoshi, Yoshizumi, SB31I-1, P1-027, P1-028, P1-057,

P1-058, P1-073, P3-058 Mizutani, K., SA51-1 Mlynczak, M., SA32-3 Mohankumar, K., P1-005, P3-073 Moldwin, M. B., SB51I-1

Moldwin, M. B., P3-052 Molodij, G., P3-096 Molodykh, S. I., P1-006 Moon, Y.-J., P1-089, P1-097 Moore, T. E., SB31-3, P3-049 Morel, B., P1-065 Morgan, H., SB21-1 Mori, S., P1-013 Morimoto, M., P1-025 Morioka, A., SB31I-2, P1-028 Morishita, R., SB42-6 Morita, S., P1-049 Morrill, J. S., SB21-6 Morris, R. J., SA41-2 Motoba, T., SA31-2, P1-100 Mukai, T., P1-063, P1-085, P1-083 Munakata, K., P1-030, P3-036, P3-106 Munoz, G., P3-024 Murakami, N., P1-043, P3-099 Murakami, T., SB21-4 Muraki, Y., SA21I-1 Murayama, Y., SA51-1 Murphy, D. J., SA41-2 Mursula, K., P1-104 Murtagh, D., SA42-2 Mustafa, F. R., P1-026, P1-086, P3-023 Nagai, T., P1-083 Nagasawa, C., P3-077, P3-100 Nagasrinivas, M. P., P1-003 Nagata, D., P1-083 Nagata, S., SB11Ｉ-2, SB11-2, SB11-1, SB11-3, SB11-4,

SB11-6, SB12I-1, SB12-4, SB21I-2, SB51-3, P1-060, P1-114

Nagatsuma, T., P3-105 Nagaya, K., SA21I-1, SB52-4 Naito, Y., SA21-4 Nakajima, A., P3-030 Nakamizo, A., SB32-6 Nakamura, M., P1-015 Nakamura, Tahei, SB11-6, P1-046, P1-114 Nakamura, Takuji, SA31-4, SA41I-3, P3-100, P3-102, P3-072 Nakamura, Toshio, SA21I-1, SB52-4 Nakano, S., P3-043 Nakatani, Y., SB51-3, SB51-4, P1-060 Nakayama, T., SA12-4 Namboodiri,K.V.S, P3-063 Narayanan, V. L., P3-071 Narita, Y., P1-079 Nariyuki, Y., SB21-3, P1-079 Narock, T., SB52I-2

Narukage, N., SB12-1, SB12-5, SB21I-1 Narumi, T., P3-036 Nayar, S. R. P., P3-075 Nerem, R. S., P1-048 Ning, B., P3-078 Niranjan, K., P1-068, P3-014 Nishi, N., P3-060 Nishida, A., Ｔ2 Nishida, K., P1-084 Nishikawa, N., SB41-7 Nishimura, K., SA52-4 Nishimura, Y., P1-040, P3-016 Nishioka, M., P1-043 Nishitani, N., P1-056, P1-057, P1-058, P3-058 Nishizuka, N., SB11-6, P1-072, P1-114 Nitta, N. V., SB31-2 Nitta, S., SB41-4 Niwano, M., P3-060 Nose, M., P3-107, P3-110 Nozaki, K., SB32-2, P1-076, P1-110, P3-039 Nozawa, Satonori, SA31-2, SA32-2, P1-059, P1-067, P1-078,

P1-082, P1-100, P3-058, P3-083, P3-097 Nozawa, Satoshi, SB11-6 Numata, Y., P3-047 Nurhayati, N., P3-082 Obara, T., SB32-6, P1-083, P3-006, P3-108 Oberoi, D., P1-071 Obridko, V. N., P1-026, P1-086, P3-023 Obuchi, Y., SB41-2, P3-041 Odagi, Y., P3-110 Offermann, D., SA32-3 Ogawa, T., SA31-4, P1-057, P1-058 Ogawa, Y., SA31-2, SA32-2, SB41-2, P1-059, P1-078, P1-082,

P1-100, P3-087, P3-097 Ogino, T., SB21-5, SB41-5, SB42I-1, SB42-6, P1-066, P3-006,

P3-026, P3-028, P3-031 Oh, S. Y., P1-087, P1-094 Ohtaka, K., P1-056, P1-085 Ohtani, S., P3-043 Okada, M., P3-041 Okada, T., P3-038, P3-084, P3-098 Okamoto, T. J., SB11-2, SB11-6 Okazaki, Y., P1-018, P3-036 Omura, Y., SB31-1, P1-081, P1-091, P3-006, P3-021, P3-034,

P3-038 Ono, T., SB31I-2, P1-027, P1-040, P1-074, P3-016, P3-038,

P3-084 Orsolini, Y. J., SA42-2 Ortland, D. A., SA41I-4 Otsuji, K., SB11-6, SB51-3, P1-060, P1-114

Otsuka, Y., SA31-4, SA31-3, SB12-2, P1-043, P3-070 Oya, H., SB31I-2 Oyama, S., SA31-2, SA32-2, P1-059, P1-067 Ozima, M., P1-103 Pacini, A. A., P1-002 Pancheva, D. V., P3-072 Pandya, N. Y., P3-065 Pant, T. K., P1-093, P3-062, P3-074, P3-075, P3-086 Panwar, V., P1-020 Papitashvili, V., P3-059 Parameswaran, K., P3-094 Park, K. S., SB41-5, P1-066 Parker, E. N., T1 Patel, D. S., P1-098 Patel, K., P1-099 Patel, R. P., P1-099 Pathan, B. M., P1-029, P3-033 Patil, C. G., P3-018 Patra, A. K., P1-023, P3-062 Paul, A., P1-050 Persiantsev, I. G., P3-002 Pilipenko, V. A., P1-088, P3-037, P3-048 Pillai, P. A., P3-073 PNST team, P3-057 Poedts, S., SB42Ｉ-2, SB52-2 Pokorna, L., SA22-6 Prasad, D. S. V. V. D., P3-014 Prasad, M. Y. S., P3-018 Price, C., P1-090 Pulkkinen, T. I., P3-025 Qiang, H., SA11-2 Rachman, A., P1-031 Rahman, M. M., P1-109 Rajaram, G., P3-018 Rajeev, K., P3-094 Rajesh, J., P1-005 Rajput, H. M., P1-010 Raju, C. S., P3-094 Ram, S. T., P3-014 Ramkumar, G., P3-086 Ramkumar, G., P3-061, P3-063 Ramkumar, T. K., P3-089, P3-090 Randall, C. E., SA12Ｉ-1 Rao, D. N., P3-089, P3-090, P3-094 Rao, K. G., SA11-5, P3-094 Rao, P. B., SA11-5 Rao, P. S. D., P1-102 Rao, P. V. S. R., P3-014 Raspopov, O., P1-022 Rathod, J., P3-018

Ratnam, D. V., P1-102 Ratnam, M. V., P3-069 Ravindran, S., P1-034, P1-061, P1-093, P3-055, P3-074,

P3-075, P3-086 Rawat, R., P1-032 Ray, S., P1-050 Raymond, J., P3-040 Reddy, R. V., P1-038 Reeves, K., P3-040 Reid, I. M., SA52-2 Renggono, F., P3-064 Richmond, A. D., SA31Ｉ-1 Rideout, W., P3-050 Roble, R. G., SA31Ｉ-1 Rodriguez, L., SB52-2 Romashets, E. P., SB22-2 Rumbold, S. T., SA21Ｉ-3 Russell, C. T., SB51I-1, SB51-1 Russell, J. M., SA41I-5 Ruzmaikin, A., SA12-5 Saar, S. H., SB12-1 Saito, A., SA31-3, SA52-4, SB12-2, P1-043, P3-070, P3-099 Saito, S., SA31-3, P1-110, P3-080 Saito, Y., P1-063, P1-083, P1-085 Saiz, E., SB52-2 Saka, O., P3-004 Sakanoi, K., SA12-1, SA51-1, P1-018 Sakanoi, T., SB41-2, P1-028, P3-041 Sakao, T., SB11-1, SB12-1, SB12-5, SB21I-1 Sakurai, A., P1-078 Sakurai, T., SB42-1, P3-012 Salah, J. E., P1-071 Sanchez, A. L., P1-041 Sapra, R., P1-020 Sarkar, S., P1-036 Sarma, A. D., P1-102 Sathishkumar, S., P3-066 Sato, K., SA42I-2, SA42I-5, SA51-2, SA52-4 Sato, M., SA12-1, P1-018 Sato, N., P1-057, P1-063, P1-074 Sato, T., SA52-4 Sato, Y., P1-074 Schlegel, K., P1-044 Schmidt, H., SA32I-1 Schmieder, B., SB52-2, P3-096 Schuch, N. J., P1-030 Schuurmans, C. J. E., SA22I-2 Schwadron, N., P3-040 Seki, K., SB41-2, P1-027, P1-073, P1-103, P3-027, P3-030,

P3-041, P3-042, P3-058

Sekii, T., SB21I-2 Selvamurugan, R., P3-033 Sen, A., P3-021 Seto, T. H., P1-013 Shanthakumaran, A., P1-106 Sharma, S., P1-010 Shepherd, G. G., SA32-3, SA32-4 Shepherd, M. G., SA32-3 Shevtsov, B. M., P3-039 Shibagaki, Y., SA51-3, P1-013, P3-092 Shibasaki, K., SB12-1 Shibata, Kazunari, SB11-2, SB11-6, SB41-6, SB41-7, SB42I-1,

SB42-4, SB51-3, SB51-4, P1-046, P1-054, P1-060, P1-072, P1-084, P1-114, P3-006, P3-035

Shibata, Kiyotaka, SA21-3, SA21-5, SA22-3 Shibata, Y., P3-077, P3-100 Shimazu, H., SB32-6 Shimizu, M., SB11-6, P1-084 Shimizu, Tohru, SB41-6, P3-054 Shimizu, Toshifumi, SB11-1, SB11-2, SB11-3, SB11-4,

SB12I-1, SB12-4, SB21I-2, P1-114 Shimojo, M., SB11-4, SB12-1, SB12-4, SB21I-2 Shimomai, T., P1-013, P3-064, P3-079, P3-092 Shinagawa, H., SA31-2, SB32-6, P1-103, P3-070 Shinbori, A., P1-040, P1-076, P3-011, P3-016, P3-017 Shindell, D. T., P1-011 Shine, K. P., SA21Ｉ-3 Shine, R., SB11-1 Shine, R. A., SB11-2, SB11-3, SB12I-1, SB21I-2 Shinohara, I., SB41-2, P1-063 Shinohara, M., P1-076, P3-039 Shiokawa, K., SA31-4, SA41I-3, P1-027, P1-056, P3-030,

P3-058 Shiota, D., SB41-7, SB42I-1, P1-084 Shishov, V. I., SB22-5 Shoji, M., P1-081 Shrivastava, A., P1-010 Shugai, J. S., P3-002 Shustarev , P. N., P3-023 Sibeck, D. G., SB41-3 Sigmond, M., SA21-2 Singer, H. J., P3-052 Singer, W., SA32-3, SA41-2 Singh, A. K., P1-099 Singh, R. P., P1-099 Singh, S. V., P1-038 Siskind, D. E., SA12Ｉ-1 Sivakumar, V., P1-095 Sivaraman, M. R., P1-061 Sivjee, A., SA52-2

Smith, A. K., SA22I-1, SA22-4 Socas-Navarro, H., SB11-4 Solanki, S. K., SA11I-3 Song, I.-S., SA51I-1 Spangehl, T., SA52-1 Spence, H., P3-040 Sreehari, C., P3-075 Sreeja, V., P1-034, P1-061, P3-074, P3-075, P3-086 Sridharan, R., SA11-5, P1-034, P1-061, P3-074, P3-075,

P3-086 Sridharan, S., SA32-1, P3-072, P3-102 Sripathi, S., P3-062 Srivani, B., P1-068 Srivastav, K. C., P1-107 Steiner, O., P1-113 Stoilova, I., P1-026, P1-086, P3-023 Strangeway, R. J., P3-030 Su, H.-T., SA12-1 Su, S.-Y., P3-003 Subaev, I. A., SB22-5 Suematsu, Y., SB11-1, SB11-2, SB11-3, SB11-4, SB12I-1,

SB12-4, SB21I-2, P1-114 Sugimoto, N., P3-076 Sugiyama, T., SB42-3 Suleiman, B., SB42-2 Summers, D., P3-034 Sumod, S. G., P3-075 Sung, S.-K., P1-066 Suparta, W., P1-007 Sutton, E. K., P1-048 Svalgaard, L., K5-2 Swain, D., P3-063 Syamsudin, F., P1-013 Tabata, Y., P1-013 Taguchi, S., P1-025 Takahashi, H., P3-072 Takahashi, K., SA12-4, P3-107 Takahashi, M., SA22-5, SA42I-2, SA42I-5, SA51-2 Takahashi, Y., SA12-1, P1-018 Takasaki, H., P1-072 Takasaki, S., SB32-1 Takashima, T., P1-027 Takayabu, Y., P3-069 Takeda, M., P3-110 Tanaka, S., P3-031 Tanaka, T., SA11-2, SB32-6, SB42-5 Tanaka, Y., P3-087 Tanaka, Y. T., P3-091 Tarbell, T., SB11-1 Tarbell, T. D., SB11-2, SB11-3, SB12I-1, SB21I-2

Taseva, T., P1-086 Tatarinov, P. V., P1-096 Taylor, M. J., SA42Ｉ-4 Terada, N., SB32-6, P1-103 Teramoto, M., P3-107 Terasawa, T., P3-091 Thampi, S., P3-074, P3-086 Thampi, S. V., P1-023 the Modeling Task Force Group, SB42I-1, P3-006 Thomas, S., P3-094 Thomasson, P., SB21-1 Thomsen, M. F., P3-013, P3-052 Tinsley, B. A., SA12I-3, SA12-2 Title, A., SB11-1 Title, A. M., SB11-2, SB11-3, SB12I-1, SB21I-2 Tiwari, C. M., P1-024 Tiwari, D., P3-062, P3-074 Tiwari, D. P., P1-024 Tjul'bashev, S. A., SB22-5 Tokumaru, M., SA11I-2, SB21-4, SB22-1, P1-047, P1-055 Tokunaga, T., P3-046 Tomikawa, Y., SA42I-2, SA42I-5, SA52-4 Tourpali, K., SA22I-2 Tripathi, D., SB12I-2 Trompier, F., P3-051 Tsubouchi, K., SB32-6, SB52-3 Tsuchiya, F., P1-028 Tsuda, T., SA32-1, SA51-4, P1-105, P3-069, P3-072, P3-079,

P3-102 Tsuda, T. T., SA31-2, SB12-2, P1-043 Tsuji, Y., P3-011 Tsuneta, S., K1-3, SB11Ｉ-2, SB11-1, SB11-2, SB11-3, SB11-4,

SB12I-1, SB12-1, SB12-4, SB21I-1, SB21I-2, P1-114, P3-012 ,

Tsuneta, Y., P1-056 Tsurutani, B. T., SB52-1, P1-081 Tsutsumi, M., SA41I-3, SA52-4 Ueda, Y., P3-038 Ueno, G., P3-043 Ueno, S., SB11-6, SB51-3, SB51-4, P1-046, P1-060, P1-114 Ueno, T., P3-047 Ugai, M., SB41-6, P3-005, P3-054 Uma, S., P1-106 Umeda, T., SB21-5, P3-020, P3-031 Umemoto, Y., P1-013 Unruh, Y. C., SA11I-3 Uozumi, T., P1-035, P3-044, P3-046, P3-047 Upadhayaya, A. K., P3-068 Urban, J., SA42-2 Usoskin, I., P1-104

Usoskin, I. G., P1-004 Usui, H., P1-091 Valdes-Galicia, J. F., P1-041 Vandas, M., SB22-2 Vargas, B., P3-024 Varotsou, A., SB31-3 Vats, H. O., P1-053 Veenadhari, B., P1-045 Velasco, V., P1-001 Verkhoglyadova, O., P1-081 Veselovsky, I. S., P3-002 Vieira, L. E. A., P1-030 Vincent, R. A., K5-1, SA52-2, P3-102 Vineeth, C., P3-074, P3-086 Voronin, N. A., SA11-4 Vourlidas, A., SB22Ｉ-1 Walker, R. J., SB52I-2 Walker, S. N., P3-032 Wan, K., SA42Ｉ-1 Wang, C., SB22-7 Wang, H., P3-053 Wang, L., SA42Ｉ-1 Wannberg, G., SB21-1 Ward, W. E., SA31I-2 Washimi, H., SA11-2 Watanabe, H., SB11-6, P1-046 Watanabe, S., SA42I-5 Watanabe, Shigeto, P3-015 Watanabe, Shingo, SA42I-2, SA51-2 Watanabe, Taiki, P1-067 Watanabe, Tetsuya, SB12-3 Watanabe, Y., P1-056 Watari, S., P1-056, P1-085, P3-046 Webb, D., P3-040 Webb, D. F., SB21-6 Weber, M. A., SB12-1 Werne, J., SA42Ｉ-1 WG 4.4, SB52Ｉ-1 Whittick, E., SB21-1 Woithe, J., SA52-2 Wu, C.-C., SB41-1 Wu, D. L., SA42I-3 Wu, Q., SA41-1 Wu, S. T., SB41-1 Xie, H., SA11-1 XRT Team, SB12-5 Xu, J., SA41-1 Yadav, M., P3-062 Yagi, M., P3-027 Yagitani, S., P3-038

Yagova, N., P1-090 Yagova, N. V., P3-037, P3-048 Yamagishi, H., P1-057 Yamamoto, M., SA31-3, P3-060 Yamamoto, M. K., SA51-3, P1-013, P3-060, P3-064 Yamamoto, T., P3-012 Yamamoto, T. T., SB42-1 Yamanaka, M. D., P1-013 Yamanouchi, T., SA52-4 Yamashita, Y., SA22-5 Yamazaki, A., SB41-2 Yang, H., P1-044 Yang, Y.-H., P1-019 Yao, Y., P1-073 Yashiro, S., SA11-1, P1-092 Yatim, B., P1-007 Yi, Y., P1-087, P1-089, P1-094 Yoden, S., SA21-4 Yokoi, N., SB22-4 Yokoyama, M., P1-009 Yokoyama, Takaaki, SB11Ｉ-2, SB11-4, SB21I-2, SB42-1,

P1-012, P1-075, P3-012 Yokoyama, Tatsuhiro, SA31-3 Yokoyama, Y., SA21I-1 Yoshida, A., P3-109 Yoshida, M., P3-091 Yoshida, S., P3-029 Yoshikawa, A., P1-076 Yoshino, S., P3-098 Yoshitaka, O., SA12-1 Young, C. A., P1-049 Yuan, Z., P3-078 Yukimatu, A. S., P1-057, P1-063 Yukimoto, S., SA21-2 Yumoto, K., SB32-1, SB51I-1, SB51I-2, SB51-1, P1-028,

P1-035, P1-076, P3-030, P3-039, P3-044, P3-046, P3-047 Yung, Y. L., SA12-5 Zaharia, S., SB32-4 Zelenyi, L. M., K4-2 Zhao, Y., SA42Ｉ-4 Zheng, X., SA12-2 Zherebtsov, G. A., P1-006 Zhou, L., SA12-2 Zhukov, A., SB52-2 Zomer, A., P1-090 Zou, S., SB22-7

MondayOctober 22

TuesdayOctober 23

WednesdayOctober 24

ThursdayOctober 25

FridayOctober 26

SaturdayOctober 27

9 AM 9:15-10:15 9:15-10:15 9:15-10:35 9:15-10:15 9:15-10:15

Opening SessionOS1 Susan K. Avery

TutorialT1 Eugene N. Parker

KeynoteK3-1 Yohsuke KamideK3-2 Janet U. Kozyra

TutorialT2 Atsuhiro Nishida

TutorialT3 Marvin A. Geller

10 10:30-12:30 10:30-12:30 10:30-12:30 10:30-12:30

KeynoteK1-1 Juerg BeerK1-2 Karin LabitzkeK1-3 Saku Tsuneta

KeynoteK2-1 Joanna D. HaighK2-2 Nat Gopalswamy

K2-3 Franz-Josef Luebken

10:50-12:10Keynote

K3-3 Mausumi DikpatiK3-4 Shoichro Fukao

KeynoteK4-1 John T. GoslingK4-2 Lev M. ZelenviK4-3 Jeffrey M. Forbes

KeynoteK5-1 Robert A. VincentK5-2 Leif SvalgaardK5-3 Claus Frohlich

11

12 PM 12:10-1:10

12:30-1:30 12:30-1:30 Lunch 12:30-1:30 12:30-1:30

Lunch Lunch Lunch Lunch

1 1:10-2:50

1:30-3:40 1:30-3:40Session

1:30-3:40 1:30-3:10

SessionSA11 Solar and Space VariabilitySB11 Observations of Solar-Terrestrial Environment I

SessionSA21 Solar Cycle and Long-term

Response ISB21 Solar Wind I

SA31 IonosphereSB31 High Energy Particles

SessionSA41 Mesosphere and Lower

ThermosphereSB41 Magnetic Reconnection and

Particle Acceleration

SessionSA51 Dynamical Coupling,Equatorial WavesSB51 Ground-basedObservation

22:50-3:50Poster, P3

3 3:25-5:05

3:40-4:40 3:40-4:40 3:40-4:40 Session

4:00-8:00 Poster, P1 Poster, P13:50-5:30Session

Poster, P3

4 Registration

SA32 Mesosphere andThermosphere

SB32 Special SessionCommemorating Prof. Kamide's

Achievements

SA52 Climate Dynamics, Radarand Optical Observations

SB52 Geomagnetic Storms andSolar Cycle Variation

4:40-6:50Session

4:40-6:50Session

4:40-6:50Session

5

SA12 Short-term Solar Influenceon Earth's Environment

SB12 Observations of Solar-Terrestrial Environment II

SA22 Solar Cycle and Long-termResponse II

SB22 Solar Wind II

SA42 Gravity Waves, LagrangianMotions

SB42 Space Weather Modeling andSimulation

5:20-6:20Discussion

66:00-8:00Ice breaker

6:30-8:30Banquet

7

8

Conference Schedule

Timetable of International CAWSES Symposium

Date

Time