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

Publication: Research - peer-reviewJournal article – Annual report year: 1992

Without internal affiliation

  • Author: Buneman, 0.

    Stanford University, United States

  • Author: Neubert, Torsten

    University of Michigan

  • Author: Nishikawa, K.I.

    University of Iowa, United States

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We present here our first results of simulating the solar wind-magnetosphere interaction with a new three-dimensional electromagnetic particle code. Hitherto such global simulations were done with 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. Our kinetic model attempts to combine the macroscopic and microscopic tasks. It relies only on the Maxwell curl equations and the Lorentz equation for particles, which are ideally suited for computers. The preliminary results shown here 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-dusk asymmetries.
Original languageEnglish
JournalI E E E Transactions on Plasma Science
Issue number6
Pages (from-to)810-816
StatePublished - Dec 1992
Externally publishedYes
CitationsWeb of Science® Times Cited: 33
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ID: 10135960