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“Plasma-neutral gas simulations
of reconnection events in cometary tails”
C. Konz, G. T. Birk, & H. Lesch2004, A&A, 415, 791-802
DOI: 10.1051/0004-6361:20031695
S. Tanuma
(Kwasan Observatory)
The formation and dynamical evolution of cometary plasma tails and magnetic boundary layers is studied by the first numerical plasma-neutral gas simulations.
Disconnection Event• “Intreplanetary gas. XXVIII. Plas
ma tail disconnection events in comets: Evidence for magnetic field line reconnection at interplanetary sector boundaried?”, Niedner & Brandt 1987, ApJ, 223, 655
• Comet Morehouse 1908c (Yorkes Observatory)
• (Top) 20:57 GMT, 1908 Sep 30
• (Bottom) 19:43 GMT, Oct 1
Disconnection Event (DE)
• “Intreplanetary gas. XXVIII. Plasma tail disconnection events in comets: Evidence for magnetic field line reconnection at interplanetary sector boundaried?”, Niedner & Brandt 1987, ApJ, 223, 655
• 1974 Jan 21
• Comet Kohoutek
• Des were also observed at the comet Halley 1985-86
Reconnection in cometary tail
Dense, cold, neutral and slab-like comet
Hot, magnetized ambient plasma flow
inflow
× Nightsidereconnection
Current sheet
Reconnection in cometary head
Dense, cold, neutral and slab-like comet
Hot, magnetized ambient plasma flow
inflow
×Dayside reconnection
Current sheet
Secure boundary
Similar Simulations• Reconnection triggered by the comet (reconnection arou
nd the comet, magnetotail; Niednet & Brandt 1979; Niednet, Ionson, & Brandt 1981; Niedner 1982; Ogino, Walker, & Ashour-Adballa 1986; Niednet & Brandt 1987; Brandt & Niednet 1987; Niedner & Schwingennschuh 1987; Ogino 1988; Brandt & Snow 2000)
• Reconnection triggered by the high velocity cloud (Konz, Birk, & Lesch 2004; Konz, Bruns, & Birk 2002)
• Reconnection in the earth’s magnetosphere (Ogino’ papers; Birk, Lesch, & Konz 2004)
• Reconnection triggered by the flux tube
Earth
• “Solar wind induced magnetic field around the unmagnetized Earth”, Birk, Lesch, & Konz 2004, A&A, 420, L15 (pdf)
• See also Ogino’s papers
High Velocity Clouds• “Dynamical evolution of t
he high velocity clouds” Konz, Birk, & Lesch 2004, ApSS, 289, 391 (pdf)
• “Dynamical evolution of high velocity clouds in the intergalactic medium”, Konz, Bruns, & Birk 2002, A&A, 391, 713: Strong radio emission around HVC complex C (pdf; fig)
New point of this paper
• Two fluid (ion and plasma)
• Collisional momentum transfer
• (Birk& Otto 1996, J. Comp. Phys., 125, 513)
• Small and many grid
• Harris-like sheet
Basic Equation (1)
Plasma continuum equation
Neutral gas continuum equation
Plasma momentum equation
Neutral gas momentum equation
Normalization by L, Alfven velocity, Alfven time, magnetic pressure
Basic Equation (2)
Plasma pressure equation
Neutral gas pressure equation
Induction equation
Constraint of momentum conservation
Classical model
Recombination/ionization
Typical parameters in solar wind at 1 AU
• L=5x10^10 cm (The extend of ionosphere of comet at 1 AU)
• No=12 cc
• Bo=5x10^-3 G
• Va=3.15x10^8 cm/s
• ta=159 s
• (Typical quantities at 1 AU)
Initial Condition (Run I)
Dense, cold, neutral and slab-like cometRho_no=1.5x10^4(no=12 cc)T_no=1
Hot, magnetized ambient plasma flowRho_min=1To=100
Vy0=-0.15 (=470 km/s); MA=15
B=Bx =Bo =0.01(=50microG)
-60<x<60-250<y<30303x703 grids
R=2
X=0
Y=30
Y=0
Y=-250X=-30 X=30
Anomalous resistivity model
• They always adopt this model. They assume a background resistivity for the first time.
Eta_=10^-5 (>eta_num=10^-6)Eta_2=0.05Jc=0.1
B, v, resistivity
T=2
T=300
T=900 T=2431
T=2372
T=1786
Anomalous resistivity sets in
Petschek reconnection starts at t=1000
Nightside reconnection
core
Jz
|B|
Results of Run I• Disconnection event (DE): Solar wind magnetic barre
r; Dayside diffusion comet’s ionosphere night side reconnection
• This process is quasi-syclic.• Since we did not include mass-loading of the solar wind
and outgasing from the comet's surface, no plasma density enhancement can be seen in the ejected tail.
• However, increased Ohmic dissipation at the pinched region can account for a brightening of the disconnected tail head.
• Including ionization processes and outgasing of neutrals is necessary to end up with a plasmoid like density enhancement of the tail plasma.
Initial Condition (Run II)
Dense, cold, neutral and slab-like cometRho_no=1.5x10^4(no=12 cc)T_no=1
Hot, magnetized ambient plasma flowRho_min=1To=100
Vy0=-0.15 (=470 km/s); MA=15
B=Bx =Bo =0.01(=50microG)
-60<x<60-250<y<30303x703 grids
R=2
X=0
Y=30
Y=0
Y=-250X=-30 X=30
Harris-type current sheet is assumed at y=25 at t=705ta in Run I. The other conditions are same with Run I.
Y=25
Run I
Second boundary
Strong current
Run I
Results of Run II
• The dayside reconnection occurs violently.
• Dayside reconnection: more dynamic, more violent, 2.5 times higher resistivity, higher reconnection rate, shorter time scale
Conclusion
• The formation and dynamical evolution of cometary plasma tails and magnetic boundary layers is studied by the first numerical plasma-neutral gas simulations.
• It is shown that collisionless interaction between the cometary envelope and the solar wind plasma leads to the formation of a magnetic barrier.
• The dynamics of the magnetotail are governed by multiple magnetic reconnection.
• If the comet encounters a heliospheric current sheet, strong disconnection events characterize the cometary plasma tail.
• But even in the case of homogeneous solar wind conditions, partial disruption of the tail is triggered by dayside reconnection.