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3D multi‐fluid MHD studies of the solar wind interaction with Mars
Author(s) -
Liu Yifan,
Nagy Andrew F.,
Groth Clinton P. T.,
DeZeeuw Darren L.,
Gombosi Tamas I.,
Powell Kenneth G.
Publication year - 1999
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/1999gl900584
Subject(s) - bow shock (aerodynamics) , venus , mars exploration program , physics , magnetohydrodynamics , solar wind , planet , astrobiology , geophysics , shock (circulatory) , plasma , shock wave , mechanics , astrophysics , medicine , quantum mechanics
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 2.7×10 25 s −1 , which is consistent with Phobos‐2 estimates.