Physics
Scientific paper
Sep 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999georl..26.2689l&link_type=abstract
Geophysical Research Letters, Volume 26, Issue 17, p. 2689-2692
Physics
28
Magnetospheric Physics: Solar Wind Interactions With Unmagnetized Bodies, Ionosphere: Planetary Ionospheres, Planetology: Solid Surface Planets: Ionospheres, Magnetospheric Physics: Numerical Modeling
Scientific paper
The interaction of the solar wind with planets with no or only very weak intrinsic magnetic fields, such as Mars and Venus, involves their ionospheres. Single fluid MHD models, which incorporate some of the important mass-loading processes, have been useful in reproducing numerous observed features at these planets, such as the location of the bow shock, but they do have obvious limitations. Our present 3D MHD model is a two-fluid one, which considers protons and the dominant heavy ions in the ionosphere, separately. We have used this model to study the interaction processes at Mars. The model results are in general agreement with the average observed bow shock shape and position and predict reasonable locations for the ionopause. The calculated oxygen escape flux down the tail was estimated to be 2.7×1025s-1, which is consistent with Phobos-2 estimates.
DeZeeuw Darren L.
Gombosi Tamas I.
Groth Clinton P. T.
Liu Yifan
Nagy Andrew F.
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