Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p21b0380b&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #P21B-0380
Physics
2756 Planetary Magnetospheres (5443, 5737, 6030), 2780 Solar Wind Interactions With Unmagnetized Bodies, 6225 Mars
Scientific paper
The lack of an intrinsic magnetic field at Venus, Mars and comets makes their interaction with the solar wind to exhibit many similarities. Among these, the formation of a magnetic barrier in front of a highly conducting obstacle and an induced magnetic tail are the most characteristic peculiarities. At Mars and comets, a sharp plasma boundary that represents the outer edge of the magnetic barrier, the Magnetic Pileup Boundary (MPB), has been identified by very clear observational signatures, including a gradient in the magnetic field magnitude (frequently observed as a sharp jump) accompanied by a decrease in the magnetic field fluctuations, and a simultaneous drastic decrease in the solar wind electron and proton densities, as the exospheric-induced ions become more important. Recently, an analysis of the 3-D magnetic field topology in the surroundings of the Martian MPB using Mars Global Surveyor magnetometer data has revealed a sudden enhancement of the field line draping exactly at the boundary itself. This feature appears to be a ubiquitous characteristic of this boundary, even when there is no obvious signature on the magnetic field magnitude. We apply the same technique to magnetometer data acquired near comets and Venus to show that this enhancement of draping is a commonplace for all weakly magnetized atmospheric bodies. As a corollary, we propose for the first time a mean to find the location of the counterpart of the MPB at Venus. Despite numerous studies on the physics of the Venusian magnetic barrier, such boundary has never been reported since there is usually no clear signature on the magnetic field magnitude.
Acuña M.
Bertucci Cesar
Connerney Jack
Crider Dana
Lin Runliang
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