Three-dimensional MHD simulations of the interaction between Venus and the solar wind

Details Three-dimensional MHD simulations of the interaction between Venus and the solar wind Three-dimensional MHD simulations of the interaction between Venus and the solar wind

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jgr...10021645c&link_type=abstract

Journal of Geophysical Research, Volume 100, Issue A11, p. 21645-21658

Physics

Plasma Physics

19

Magnetospheric Physics: Solar Wind Interactions With Unmagnetized Bodies, Planetology: Solid Surface Planets: Interactions With Particles And Fields, Space Plasma Physics: Numerical Simulation Studies, Planetology: Solid Surface Planets: Magnetic Fields And Magnetism

Scientific paper

We have developed a three-dimensional, single-fluid, MHD code which has successfully simulated the major qualitative features of the Venus-solar wind interaction. A bow shock forms at a height above the ionosphere close to that deduced from Pioneer Venus Orbiter (PVO) observations. The bow shock shows an asymmetry in the terminator plane qualitatively similar to results obtained from PVO data analyses. The magnetic field drapes over the planet and forms a two-lobed magnetotail. The magnetic field configuration near the planet is very similar to that recorded by PVO as well. We model the Venus obstacle as a hard, conducting sphere. We simulate the case in which the IMF is tilted with respect to the incoming solar wind velocity at approximately the Parker spiral angle; this is the first simulation of this particular case which includes all spatial regions of the interaction.

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