Martian obstacle and bow shock: origins of boundaries anisotropy

Details Martian obstacle and bow shock: origins of boundaries anisotropy Martian obstacle and bow shock: origins of boundaries anisotropy

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004adspr..33.2222v&link_type=abstract

Advances in Space Research, Volume 33, Issue 12, p. 2222-2227.

Physics

7

Mars, Obstacle To Solar Wind, Bow Shock, Modeling, Anisotropy, Ram Pressure Dependence

Scientific paper

The origin of the anisotropy in the shape of the Martian obstacle and bow shock is analyzed using Mars Global Surveyor observations. The influence of MHD or ion pick-up effects on Martian obstacle position was to be small found, however, localized Martian crustal magnetization increases the thickness of the downstream planetary magnetotail by 500-1000 km in agreement with earlier Phobos 2 observations. A new analytical model is presented for Martian obstacle shape variation for different solar wind ram pressure. Elongation of the Martian BS cross-section in the direction perpendicular to IMF was confirmed while the shift of this cross section in the +Y direction of Martian interplanetary medium reference frame was discovered. The shift of BS cross section in the direction of interplanetary electric field was not revealed thus not conforming the idea that mass-loading play some role in BS control.

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