Studies on the 2002 July 23 Flare with RHESSIAyumi ASAI

Solar Seminar, 2003 June 2

RHESSI ()Reuven Ramaty High Energy Solar Spectrospic ImagerLaunched on 2002 Feburary 5

weight : 290kglength : 2.2m(solar panel : 5.7m)cost : 70M$

RHESSIenergy range : 3 keV 17 MeVimagingmaximum spatial resolution : beam size : 3.3 FWHMspectroscopyhigh spectral resolution : 1~10 keV

2002 July 23 Flare 2002-July-23 00:15UT GOES X4.8 NOAA 0039 (near south-east limb)Ha image taken with Sartorius TelescopeGOES fluxNoRH 34GHzNoRH 17GHz00:0001:0002:00

EUV(195)EUV (195)images obtained with TRACEEastWest

Paper ListThe Determination and Use of Mean Electron Flux Spectra in Solar Flares J.C. BrownThe Injected Power in Solar Flare Bremsstrahlung-Producing Electrons - Death to the 'Low Energy Cutoff A.G. EmslieRHESSI Imaging Spectroscopy of the Large Gamma-Ray Flare of July 23, 2002 A.G. EmslieH-alpha line polarization in the major flare of 2002 July 23 I. Observations and data analysis N. FirstovaWhy there was no Solar Energetic Particle Event Associated with the RHESSI Flare of 2002 July 23? N. GopalswamyElectron Bremsstrahlung Hard X-ray Spectra, Electron Distributions and Energetics in the 2002 July 23 Solar Flare G.D. HolmanFirst gamma-ray images of a solar flare G.J. Hurford Explanations for Deviations from Power-Law Behavior in the Hard X-ray Spectrum of the July 23, 2002 Solar Flare E.P. KontarHard X-ray sources and motions in the July 23, 2002 gamma-ray flare S. Krucker Bob Lin's opus Implications of RHESSI Neutron-Capture Line Measurements on the Photospheric 3He/H ratio and Particle Scattering in the Coronal Magnetic Loop R.J. Murphy Regularized Dynamic Electron Flux Spectra in the July 23, 2002 Solar Flare M. PianaHigh-resolution observation of the solar positron-electron annihilation line G.H. Share Directionality of flare-associated alpha-particles at the Sun G.H. ShareHigh-Resolution Spectroscopy of Gamma-Ray Lines from the X-Class Solar Flare of 23 July, 2002 D.M. SmithRHESSI observation of the 1809 keV line from Galactic 26Al D.M. Smith Radio and hard X-ray images of high-energy electrons in a compact X-class solar flare S.M. White17 papers!

Paper ListThe Determination and Use of Mean Electron Flux Spectra in Solar Flares J.C. BrownThe Injected Power in Solar Flare Bremsstrahlung-Producing Electrons - Death to the 'Low Energy Cutoff A.G. EmslieRHESSI Imaging Spectroscopy of the Large Gamma-Ray Flare of July 23, 2002 A.G. EmslieH-alpha line polarization in the major flare of 2002 July 23 I. Observations and data analysis N. FirstovaWhy there was no Solar Energetic Particle Event Associated with the RHESSI Flare of 2002 July 23? N. GopalswamyElectron Bremsstrahlung Hard X-ray Spectra, Electron Distributions and Energetics in the 2002 July 23 Solar Flare G.D. HolmanFirst gamma-ray images of a solar flare G.J. Hurford Explanations for Deviations from Power-Law Behavior in the Hard X-ray Spectrum of the July 23, 2002 Solar Flare E.P. KontarHard X-ray sources and motions in the July 23, 2002 gamma-ray flare S. Krucker Bob Lin's opus Implications of RHESSI Neutron-Capture Line Measurements on the Photospheric 3He/H ratio and Particle Scattering in the Coronal Magnetic Loop R.J. Murphy Regularized Dynamic Electron Flux Spectra in the July 23, 2002 Solar Flare M. PianaHigh-resolution observation of the solar positron-electron annihilation line G.H. Share Directionality of flare-associated alpha-particles at the Sun G.H. ShareHigh-Resolution Spectroscopy of Gamma-Ray Lines from the X-Class Solar Flare of 23 July, 2002 D.M. SmithRHESSI observation of the 1809 keV line from Galactic 26Al D.M. Smith Radio and hard X-ray images of high-energy electrons in a compact X-class solar flare S.M. White

Imaging4 HXR sources3 footpoint sources (> 30keV)1 coronal sources (

HXR Sources

Evolution of HXR Sourcescountvelocityf1f3

Radio SourcesRadio data : Nobeyama NoRH

White et al. (2003) ApJ

TRACE12-20keV12-20keV100-150keV17GHz17 GHz sources are co-spatial with coronal HXR sources

g-Ray ImagingThis flare is the first, and the only one so far, g-ray line eventdirect indication of the spatial properties of accelerated ions near the sun2.223 MeV line narrow deuterium line (neutron capture)dense plasma (chromosphere)red-shifted precipitationHurford et al. (2003) ApJ

g-Ray Linesion accelerationcollisions with the solar atmosphereexcited nucleiemit prompt nuclear de-excitation linessecondary processneutron capture line (2.223 MeV)positron-annihilation line (511 keV)

Imaging of g-Ray Sourcesun

No Brightening in Ha1s circleerror : 6

Discussions2.2 MeV source was found to be displaced from the main bright pointthere are significant differences in location and/or morphology between the electron- and ion-associated sourcesion- and electron-light curves are similar to each othercommon acceleration process

Spectroscopyintegrated photon flux spectra :10-300 keVfittingisothermal + double power low (nonthermal)electron flux distributionthin-target / thick-targetenergy contentHolman et al. (2003) ApJ

Fitting10keV100keV

Evolution of T / EMtemperatureemission measureGOES

Thick-Targetelectron indices

EnergeticsGOESRHESSInonthermal

Discussionsfitting of nonthermal electron : double poewr law distribution with low energy cut-off : 20-40 keVminimum total energy deposited by nonthermal electrons : 2.61031 ergcomparable to thermal energy inputrequire imaging spectroscopy

Imagin SpectroscopyEvolution of spectra at 4 HXR sourcesTemperature, Emission measureEmslie et al. (2003) ApJNSMC

fittingC : thermalN, S, M : nonthermal

coronal source (C)temperature KEM Jsofter spectral index than footpoint sources (N,S,M)TEM

SummaryFlare studies with RHESSIImaging, Spectroscopy

other big flares ?2003 Mar 17/182003 May 27/28/29

18th paper on July 23, 2002 flare (by Asai et al.) ?

Double Power Lowindicessingle power lawbreak energy