Physics
Scientific paper
Jan 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....97.1017z&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 97, Jan. 25, 1992, p. 1017-1025.
Physics
17
Atmospheric Pressure, Dynamic Pressure, Mars Atmosphere, Planetary Ionospheres, Solar Planetary Interactions, Solar Wind, Venus Atmosphere, Electron Density Profiles, Electron Energy, Ion Temperature, Ionospheric Temperature, Radio Occultation, Solar Activity Effects
Scientific paper
Radio occultation measurements of electron density profiles from Mariner 6 and 7, the Mariner 9 extended mission, and the U.S. Viking orbiters, together with model ion and electron temperature profiles, are used to derive thermal pressure profiles in the Mars ionosphere. The comparison of the Mars peak ionosphere pressure with the incident solar and dynamic pressure suggests that at solar maximum the Mars ionosphere, like that of Venus, should generally be sufficient to balance the incident solar wind pressure. At solar minimum, when the ionosphere is weakest and the solar wind dynamic pressure is highest, only the peak pressures at high solar zenith angles (SZAs) at Mars appear to be strong enough to balance the incident solar wind pressure. This is similar to the situation at Venus at solar minimum.
Luhmann Janet G.
Zhang Martina H. G.
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