Solar wind flow about the terrestrial planets. II - Comparison with gas dynamic theory and implications for solar-planetary interactions

Details Solar wind flow about the terrestrial planets. II - Comparison with gas dynamic theory and implications for solar-planetary interactions Solar wind flow about the terrestrial planets. II - Comparison with gas dynamic theory and implications for solar-planetary interactions

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983jgr....88...19s&link_type=abstract

Journal of Geophysical Research, vol. 88, Jan. 1, 1983, p. 19-35.

Physics

65

Bow Waves, Gas Dynamics, Shock Wave Propagation, Solar Terrestrial Interactions, Solar Wind, Terrestrial Planets, Earth Magnetosphere, Magnetohydrodynamic Flow, Mars Atmosphere, Planetary Ionospheres, Plasma-Particle Interactions, Venus Atmosphere, Planets, Terrestrial Planets, Solar Wind, Flow, Comparisons, Gases, Dynamics, Theoretical Studies, Interactions, Calculations, Observations, Bow Shock, Models, Patterns, Magnetopause, Venus, Mars, Altitude, Magnetosphere, Pressure, Viking 1 Lander, Ionosphere, Io

Scientific paper

Bow shock models are employed to determine and compare the solar wind flows about Venus, Mars, and the earth. Initially, gas dynamic theory predictions are compared with the large data base available for the near-earth environment. The observed shape and location of the magnetopause proved sufficient for predicting the average dayside bow shock position to within 2% error. Use of the same gas dynamics theory produced highly disparate results for the flows past Venus and Mars. A variation of 510-1000 km altitude (high) for the solar wind-obstacle interface was found for Mars, thus requiring the presence of an effective magnetic moment of within 0.6 of 1.4 x 10 to the 22nd G/cu cm in the Martian magnetosphere, consistent with Viking data. The Venus bow wave was calculated to be closer to the planet than possible with a purely ionospheric interaction, indicating that solar wind-neutral atmosphere interactions in the lower ionosheath must necessarily be included in a gas dynamic modeling of the Venus obstacle to the solar wind.

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