HR: 11:55h
AN: SH42A-07    [Abstracts]
TI: Structure of the nightside plasma flows and magnetic fields in the induced magnetosphere of Mars
AU: * Maezawa, K
EM: maezawa@stp.isas.jaxa.jp
AF: Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AU: Kubota, Y
EM: kubota@stp.isas.jaxa.jp
AF: Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AU: Jin, H
EM: jin@nict.go.jp
AF: Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AB: We have numerically simulated the structure of the plasma flows and magnetic fields in the induced magnetosphere of Mars. The simulation is based on the MHD code but the effects of non-MHD terms can be quantitatively evaluated from the results. The spatial resolution of the simulation is high (the smallest vertical mesh size is 5km in the ionosphere) and both the chemical reaction and dynamical processes operating in the day as well as night time ionosphere are well represented by the code. We found that two competing processes contribute to the maintenance of the nightside ionosphere. One is the downward plasma supply from the magnetotail. The ionospheric plasma (mainly O+ and O2+ ions plus small amount of CO2+) outflowing from the dayside ionosphere is accelerated tailward by magnetic tension and then pushed toward the tail center by the JxB force. The increase of plasma pressure at the tail center produces a downward plasma flow to supply plasma to the nightside ionosphere. This process is the most important to produce and maintain the ionosphere on the nightside above 200 km height. On the other hand, the night side ionosphere below 200 km can be maintained by weak ionization rate assumed and by horizontal ionospheric convection from dayside. . The plasma flow pattern and ion density distribution in the induced magnetotail of Mars strongly depends on the IMF magnitude. When IMF is weak, the structure is axially symmetric and a large ring-shaped plasma vortex is produced behind the planet. On the other hand, when IMF is large, a strongly asymmetry exists between the distributions in two orthogonal plains, that is, between the x-y plane and x-z plane. (The coordinate system is taken such that the x-axis is directed toward the sun and the x-y plane contains IMF.) In the x-y plane, a three-ray structure is observed: Two boundary rays are produced by ions escaping parallel to the field lines that are severely draped around the planet. .On the other hand, the central ray is produced by the ions that have been accelerated tailward by magnetic tension and pushed toward the tail axis by the JxB force. The density structure in the x-z plane has only a central ray that is produced by converging flows towards the tail axis. We also estimated the total amount of escaping ions for each ion species and traced the location of the peak flux behind the planet as a function of solar wind parameters.
DE: 2451 Particle acceleration
DE: 2459 Planetary ionospheres (5435, 5729, 6026)
DE: 2463 Plasma convection (2760)
DE: 2467 Plasma temperature and density
DE: 2481 Topside ionosphere
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005