Computer Science
Scientific paper
Nov 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991p%26ss...39.1493d&link_type=abstract
Planetary and Space Science (ISSN 0032-0633), vol. 39, Nov. 1991, p. 1493-1510.
Computer Science
22
Magnetopause, Mars Atmosphere, Planetary Magnetic Fields, Planetary Magnetospheres, Shock Fronts, Interplanetary Magnetic Fields, Magnetic Moments, Solar Wind
Scientific paper
Phobos-2 plasmagrams and magnetograms are used here to identify the shock front, transition region, and magnetopause crosses for Mars. The Martian magnetic moment is estimated to be 1.35 +/- 0.03 x 10 exp 12 T-cu m. The dipole axis is inclined at an angle of 12 +/- 3 deg to the rotation axis and the north magnetic pole is in the Southern Hemisphere. The energy density of the intrinsic magnetic field is 1.2 x 10 exp -9 erg, exceeding the energy density of the ions by 13 times at 870 km altitude. The magnetic field, not the ionosphere, is the real obstacle to solar wind near Mars when P(sw) is 5 x 10 exp -9 dyn/sq cm or less. The ratios of the flux in the tail and the transverse B(perpendicular) IMF components differ considerably for weak-intensity B(perpendicular). The dependence of the tail topology on the planetary corotation with the inclined magnetic dipole, the reconnection process between the intrinsic dipole field and the Bz component of the IMF on the dayside, and the solar wind pressure are shown.
Dolginov Sh. Sh.
Zhuzgov L. N.
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