Other
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sm32d06k&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SM32D-06
Other
5421 Interactions With Particles And Fields, 5443 Magnetospheres (2756), 6225 Mars
Scientific paper
Comparison of Phobos 2 magnetic field data in the Martian magnetotail during the circular orbit phase of the mission with the Pioneer Venus Orbiter data collected throughout the magnetotail of Venus has not revealed any significant difference in the structure of their induced magnetotails. Thus, at the distance of 9600 km from Mars, the magnetic fields related to the localized regions of strongly magnetized crust tend to balance each other. At the same time, analysis of the solar zenith angle where the solar wind proton flux terminates in the Martian magnetotail has shown clustering with a solar wind ram pressure dependence. The proton termination is observed by Phobos 2 at around 130° ~solar zenith angle from the orbits when the solar wind ram pressure was less than 10-8~ dyn/cm2. The boundary crossings are scattered around 145-150° ~for solar wind ram pressure exceeding 10-8~ dyn/cm2. When these boundary crossings are mapped to where they would occur at the terminator plane, the altitudes expected are 3500 km and 1500 km for the low and high pressure cases, respectively. Analysis of the magnetic field of an inhomogeneously magnetized spherical shell of radius 3400 km, which simulates the Martian crust, has shown that these altitudes correspond to the transition between ``non-local" and ``local" effects of the crustal magnetization. Analysis of magnetotail data from Mars Global Surveyor during AB 1 and SPO 1 confirms the existence a bimodal distribution in the tail location of the magnetic pileup boundary.
Acuña Mario Humberto
Breus Tamara K.
Crider Dana Hurley
Krymskii Alexander M.
Lin Robert P.
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