Quantitative model of the Martian magnetopause shape and its variation with the solar wind ram pressure based on Phobos 2 observations

Details Quantitative model of the Martian magnetopause shape and its variation with the solar wind ram pressure based on Phobos 2 observations Quantitative model of the Martian magnetopause shape and its variation with the solar wind ram pressure based on Phobos 2 observations

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997jgr...102.2147v&link_type=abstract

Journal of Geophysical Research, Volume 102, Issue A2, p. 2147-2156

Physics

13

Interplanetary Physics: Solar Wind Plasma, Magnetospheric Physics: Magnetospheric Configuration And Dynamics, Magnetospheric Physics: Solar Wind Interactions With Unmagnetized Bodies

Scientific paper

A model of the Martian magnetopause is developed for the period of maximum solar activity which simultaneously describes (1) the observed relation between the solar wind ram pressure ρV2 and the magnetopause position in the magnetotail, (2) the observed relation between ρV2 and the flaring angle, and (3) a few magnetopause crossing observations above the day side of the planet. The shape of the magnetopause is determined from the equation of pressure balance across this boundary when both the magnetic pressure (with a planetary magnetic moment of (0.8-1.0)×1022 G cm3) and the ionospheric pressure are taken into account in the planetary magnetosphere. The specific feature of the model is the ``stagnation'' of the subsolar magnetopause when the ram pressure increases to higher values (>=6×10-9 dyn cm-2).

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