Computer Science
Scientific paper
Sep 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992adspr..12..191l&link_type=abstract
(Recent results on Mars and Venus; Proceedings of Symposium 3 and the Topical Meetings of the Interdisciplinary Scientific Commi
Computer Science
3
Mars (Planet), Planetary Magnetic Fields, Solar Planetary Interactions, Solar Wind, Venus (Planet), Magnetosheath, Planetary Magnetospheres, Planetary Magnetotails, Radiation Pressure, Solar Cycles, Solar Protons
Scientific paper
Comparisons are made of observations of features related to the solar wind interaction with Mars and with Venus, such as bow shocks, magnetospheres, magnetotails, ion environments, and ionosphere properties. It is shown that there is a great deal of similarity between the two obstacles to the solar wind, such as the proximity of the bow shocks to the planets and their solar cycle variations; the piled-up and draped magnetic fields in the magnetosheaths, which resemble the gas dynamic model; the similarly draped fields in the induced magnetotails; the occurrence of (possibly asymmetrically distributed) picked-up planetary ions in the wake and cold plasma 'clouds' near the ionopause; and the lack of a clear ionopause in the ionosphere density profile when the solar wind pressure exceeds the ionosphere thermal pressure at an altitude of about 200 km. The differences include the greater width of the bow shock at Mars.
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