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Detailed Reference Information |
Cable, S. and Steinolfson, R.S. (1995). Three-dimensional MHD simulations of the interaction between venus and the solar wind. Journal of Geophysical Research 100: doi: 10.1029/95JA02174. issn: 0148-0227. |
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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. ¿ American Geophysical Union 1995 |
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Abstract |
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Keywords
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 |
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Publisher
American Geophysical Union 2000 Florida Avenue N.W. Washington, D.C. 20009-1277 USA 1-202-462-6900 1-202-328-0566 service@agu.org |
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