Physics
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsa31a..04h&link_type=abstract
American Geophysical Union, Spring Meeting 2004, abstract #SA31A-04
Physics
2740 Magnetospheric Configuration And Dynamics, 2753 Numerical Modeling, 2756 Planetary Magnetospheres (5443, 5737, 6030), 2784 Solar Wind/Magnetosphere Interactions, 6225 Mars
Scientific paper
Under quiet solar wind conditions, the strong surface magnetic field on Mars can modify the plasma inside the bow shock, and lead to the formation of mini-magnetospheres. The crustal magnetic field has no effect on the bow shock though. 3D multi-fluid simulations are used to study the effects of pressure pulses associated with storm conditions, on the structure of the inner Martian magnetosphere. The increased dynamic pressure of the solar wind pushes the bow shock closer to the surface, into a region where stronger magnetic fields can have substantial influence on the plasma. This can also lead to enhanced ionospheric outflow. Ionospheric outflow rates down the tail are calculated for a range of solar wind conditions and crustal magnetic field orientations.
Harnett Erika M.
Paty Carol
Winglee Robert M.
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