Three-Dimensional Global Hybrid Simulation of the Bow Shock

Details Three-Dimensional Global Hybrid Simulation of the Bow Shock Three-Dimensional Global Hybrid Simulation of the Bow Shock

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsm52b0574l&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SM52B-0574

Statistics

Computation

2154 Planetary Bow Shocks, 2728 Magnetosheath, 2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions, 7839 Nonlinear Phenomena

Scientific paper

A 3-D global-scale hybrid code is developed for simulation of the bow shock and the dayside magnetosphere. A spherical, (r, θ , φ ), coordinate system is utilized in the simulation. The code is developed by generalizing our previous 2-D code [e.g., Swift, GRL 22, p.311, 1995; Lin, 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= 3RE to 20 RE. 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.

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