3D MHD simulations of the heliosphere-VLISM interaction

Details 3D MHD simulations of the heliosphere-VLISM interaction 3D MHD simulations of the heliosphere-VLISM interaction

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..823m&link_type=abstract

The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 823-826 (1999).

Physics

11

Solar Wind Plasma, Sources Of Solar Wind, Physical Properties

Scientific paper

We present results of a global 3D MHD simulation of the interaction of the solar wind with the very local interstellar medium (VLISM). Three different cases are studied: purely hydrodynamic, MHD without charge exchange and MHD with charge exchange with the VLISM neutrals. Latitudinal differences in the solar wind are included as well as the solar cycle dependence of the Interplanetary Magnetic field (IMF). The latitudinal variation in the solar wind causes the polar termination shock at a considerably larger distance than in the ecliptic at the same angle with respect to the VLISM direction. As expected, the presence of magnetic pressure in the VLISM moves the termination shock inward, as does the presence of charge exchange with the neutrals.

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