Origin of MGS-Observed Electron Flux Enhancements Using 3D Multi-Fluid Simulations of the Martian Solar Wind Interaction

Details Origin of MGS-Observed Electron Flux Enhancements Using 3D Multi-Fluid Simulations of the Martian Solar Wind Interaction Origin of MGS-Observed Electron Flux Enhancements Using 3D Multi-Fluid Simulations of the Martian Solar Wind Interaction

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p51b1409u&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #P51B-1409

Physics

2700 Magnetospheric Physics (6939), 2784 Solar Wind/Magnetosphere Interactions, 6225 Mars

Scientific paper

Previously we reported a discovery of a seasonal, nighttime clustering of particle enhancements on the Mars Global Surveyor electron flux data at low-energy levels observed over a localized geographical region in the southern hemisphere of Mars. This enhancement is likely the result of the transport of photoelectrons produced above the crustal magnetic sources on the dayside of Mars, to the magnetotail on the nightside of Mars. The transport would occur along the lines of the reconnected Interplanetary Magnetic Field (IMF). In this study, we explore the origin of the observed electron flux enhancements using three-dimensional multi- fluid simulations of the Martian solar wind interaction. Using the model, the magnetic field configuration and plasma distribution around Mars is reproduced for typical solar wind conditions and crustal field orientations. The results are compared to the observations, and consequently the possible role of magnetic reconnection between the draping IMF and the crustal fields in the observed electron enhancements is discussed.

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