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The intrinsic magnetic field and solar-wind interaction of MarsThe Venus-like interaction between the solar wind and the atmosphere of Mars is examined. The bow shock and magnetosheath of Mars indicate the presence of an obstacle to the solar wind that is somewhat larger than the size of the planet and its observed ionosphere, and also relatively larger than the Venus obstacle under comparable conditions. The intrinsic magnetic field of Mars must be no greater than 1.5 x 10 exp 12 T/cu m, or about 0.0001 times as strong as that of the earth to produce an obstacle of such small size. At least for solar minimum conditions, like those prevailing at the time of the Viking Landers, the ionospheric plasma (thermal) pressure is insufficient to balance the incident solar-wind pressure by itself. The ion and electron temperatures in the Martian ionosphere indicate the presence of local horizontal magnetic fields and heat sources in excess of solar radiation alone.
Document ID
19930043886
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Luhmann, J. G.
(NASA Headquarters Washington, DC United States)
Russell, C. T.
(California Univ. Los Angeles, United States)
Brace, L. H.
(Michigan Univ. Ann Arbor, United States)
Vaisberg, O. L.
(Russian Academy of Sciences, Space Research Inst. Moscow, Russia)
Date Acquired
August 16, 2013
Publication Date
January 1, 1992
Publication Information
Publication: In: Mars (A93-27852 09-91)
Publisher: University of Arizona Press
Subject Category
Lunar And Planetary Exploration
Accession Number
93A27883
Funding Number(s)
CONTRACT_GRANT: NAGW-1347
Distribution Limits
Public
Copyright
Other

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