Characteristics of the Marslike limit of the Venus-solar wind interaction

Details Characteristics of the Marslike limit of the Venus-solar wind interaction Characteristics of the Marslike limit of the Venus-solar wind interaction

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jgr....92.8545l&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 92, Aug. 1, 1987, p. 8545-8557.

Physics

79

Planetary Ionospheres, Plasma Interactions, Solar Planetary Interactions, Solar Wind, Venus Atmosphere, Dynamic Pressure, Electron Energy, Ion Temperature, Ionopause, Plasma Pressure, Plasma Waves, Viking Spacecraft, Venus, Solar Wind, Interaction, Comparisons, Ionosphere, Pressure, Spacecraft Observations, Pioneer Venus Orbiter, Pvo Mission, Bow Shock, Altitude, Density, Gradients, Magnetic Fields, Dayside, Temperature, Ions, Dynamics, Viking Missions

Scientific paper

The response of the Venus ionosphere to the solar wind when the latter exceeds the peak thermal pressure in the Venus ionosphere is characterized on the basis of observations from the Pioneer Venus Orbiter. At these times, the Venus ionosphere becomes increasingly magnetized until the total ionospheric pressure matches that of the solar wind. The ionopause becomes less distinct and asymptotically approaches a limiting altitude of about 220 km for extremely high pressures. When the ionopause is low, the hot regions of electrons which occurs within the ionopause gradient extends to lower altitudes. The ion temperatures show little change, and there is no discernible increase in plasma wave activity at the ionopause. The Venus observations at high dynamic pressure provide a framework for reassessing the available Mars observations. In particular, this study shows that solar wind standoff without sufficient ionospheric plasma pressure cannot by itself be used as evidence for a planetary magnetic field.

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