Comparative interactions of the ionospheres of Mars and Venus with the solar wind

Details Comparative interactions of the ionospheres of Mars and Venus with the solar wind Comparative interactions of the ionospheres of Mars and Venus with the solar wind

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsa33c..01m&link_type=abstract

American Geophysical Union, Spring Meeting 2007, abstract #SA33C-01

Physics

2780 Solar Wind Interactions With Unmagnetized Bodies, 6225 Mars, 6295 Venus, 7811 Discontinuities (2109)

Scientific paper

When dealing with the general problem of the interaction of a fast-flowing magnetized plasma with a neutral gas environment, the comparison of the interaction of the solar wind with the atmospheres of Mars and Venus is obviously of high relevance, in particular for the understanding of the loss of volatiles. Their environment consists of characteristic boundaries separating regions with very different plasma conditions and dynamics (upstream region, collisionless shock, magnetosheath, "induced" magnetosphere, ionosphere, tail, plasma sheet). The most important features are the formation of a magnetic barrier in front of the highly conducting ionosphere and an induced magnetic tail. The outer edge of the magnetic barrier on the dayside appears as a sharp boundary, reported from the magnetometer of Mars Global Surveyor and Venus Express. Recent results from the IMA mass spectrometer onboard Mars Express and Venus Express also offers us the unique opportunity to compare the plasma regimes at both planets with the same ion instrument. Recent achievements on this topic are presented.

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