HR: 1330h
AN: SM52B-0574    [PDF]
TI: Three-Dimensional Global Hybrid Simulation of the Bow Shock
AU: * Lin, Y
EM: ylin@physics.auburn.edu
AF: Auburn University, Physics Department, 206 Allison Laboratory, Auburn, AL 36849-5311 United States
AU: Wang, X
EM: xywang@physics.auburn.edu
AF: Auburn University, Physics Department, 206 Allison Laboratory, Auburn, AL 36849-5311 United States
AB: A 3-D global-scale hybrid code is developed for simulation of the bow shock and the dayside magnetosphere. A spherical, $(r, \theta, \phi)$, coordinate system is utilized in the simulation. The code is developed by generalizing our previous 2-D code [e.g., Swift, {\it GRL} 22, p.311, 1995; Lin, {\it PSS} 50, p.577, 2002] to 3-D. In the hybrid code, the solar wind and outer magnetospheric ions are treated as discrete particles, and the electrons are treated as a massless fluid. In the simulation, the bow shock forms by interaction between the supersonic solar wind and the geomagnetic dipole field. The simulation domain contains plasma regions from the geocentric distance of $r= 3R_E$ to $20 R_E$. Massively parallel computation is used in the simulation. Our previous 2-D simulations showed the presence of various electromagnetic waves near the quasi-parallel and quasi-perpendicular shocks, and the formation of diamagnetic cavities in the foreshock and downstream regions of parallel and quasi-parallel shocks due to the interaction between backstreaming ion beams and the incoming solar wind plasma. In this presentation, our preliminary 3-D simulations of the kinetic structure of the bow shock will be shown, and the results will be compared with the previous 2-D simulations.
DE: 2154 Planetary bow shocks
DE: 2728 Magnetosheath
DE: 2753 Numerical modeling
DE: 2784 Solar wind/magnetosphere interactions
DE: 7839 Nonlinear phenomena
SC: SPA - Magnetospheric Physics [SM]
MN: 2003 Fall Meeting