Solar wind-magnetosphere interaction as simulated by a 3D, EM particle code

Details Solar wind-magnetosphere interaction as simulated by a 3D, EM particle code Solar wind-magnetosphere interaction as simulated by a 3D, EM particle code

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ppcn.conf..285b&link_type=abstract

In ESA, Fourth International Toki Conference on Plasma Physics and Controlled Nuclear Fusion p 285-288 (SEE N94-22624 05-75)

Physics

Plasma Physics

Computerized Simulation, Plasma-Electromagnetic Interaction, Solar Wind, Three Dimensional Models, Magnetohydrodynamics, Plasma-Particle Interactions, Solar Magnetic Field, Stellar Magnetospheres

Scientific paper

The results of simulating the solar wind-magnetosphere interaction with a three dimensional, electromagnetic (EM) particle code are presented. Hitherto such global simulations were done with magnetohydrodynamic (MHD) codes while lower dimensional particle or hybrid codes served to account for microscopic processes and such transport parameters as have to be introduced ad hoc in MHD. The kinetic model combines macroscopic and microscopic tasks. It relies only on the Maxwell curl equations and the Lorentz equation for particles. The preliminary results are for an unmagnetized solar wind plasma streaming past a dipolar magnetic field. The results show the formation of a bow shock and a magnetotail, the penetration of energetic particles into cusp and radiation belt regions, and dawn to dusk asymmetries.

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