Physics
Scientific paper
Jan 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....97.1027s&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 97, Jan. 25, 1992, p. 1027-1035.
Physics
29
Atmospheric Models, Mars Atmosphere, Planetary Ionospheres, Planetary Magnetic Fields, Solar Planetary Interactions, Atmospheric Pressure, Dynamic Pressure, Electron Density Profiles, Magnetic Field Configurations, Solar Wind
Scientific paper
An improved model of the Martian ionosphere which allows the magnetic field to have any direction in the horizontal plane is presented, as well as results of calculations for several different intrinsic magnetic field strengths and directions. When the solar wind dynamic pressure exceeds the Martian ionospheric thermal pressure, the plasma motion is weakly downward throughout the ionosphere for the case of no intrinsic magnetic field, but when the intrinsic and induced fields are in opposite directions, the plasma flow tends to converge toward the current sheet. As a consequence of this convergence, the plasma density is somewhat enhanced near the current sheet, which is located near an altitude of 170 km. The ionosphere above an altitude of about 190 km is not significantly affected by the existence of an intrinsic field as weak as 60 nT.
Cravens Thomas E.
Shinagawa Hiroyuki
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