Solar wind-magnetosphere interaction as simulated by a 3D, EM particle codeThe 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.
Document ID
19940018201
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Buneman, O. (Stanford Univ. CA, United States)
Nishikawa, Ken-Ichi (Iowa Univ. Iowa City., United States)
Neubert, T. (Michigan Univ. Ann Arbor., United States)
Date Acquired
September 6, 2013
Publication Date
May 1, 1993
Publication Information
Publication: ESA, Fourth International Toki Conference on Plasma Physics and Controlled Nuclear Fusion