Investigation of the structure of the Martian Magnetic Pileup Region using High Resolution 3D multi-fluid Simulations

Details Investigation of the structure of the Martian Magnetic Pileup Region using High Resolution 3D multi-fluid Simulations Investigation of the structure of the Martian Magnetic Pileup Region using High Resolution 3D multi-fluid Simulations

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh43a1146h&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH43A-1146

Physics

2431 Ionosphere/Magnetosphere Interactions (2736), 2724 Magnetopause And Boundary Layers, 2753 Numerical Modeling, 2780 Solar Wind Interactions With Unmagnetized Bodies, 6225 Mars

Scientific paper

New 3D multi-fluid simulations of the solar wind interaction at Mars, with resolution of 40 km are, for the first time, able to resolve the structure of the magnetic pileup region (MPR) around Mars. Finite gyro-radius affects can be seen at the magnetic pileup boundary (MPB), leading to a pressure enhancement of oxygen ions at the MPB with no corresponding enhancement seen in the hydrogen ion population. The simulations are able to capture the changes in the MPB location and the MPR structure caused by the magnetic anomalies. The presence of the magnetic anomalies also leads to the formation of multiple cusp regions. Enhanced solar wind access is associated with the cusps as well as a lower altitude for the ionopause. In neighboring regions, ionospheric outflow is enhanced. Spectrograms generated from the simulation results show trapped ion populations associated with closed magnetic field geometries.

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