Four Martian Years Of Nightside Upper Thermospheric Mass Densities From Electron Reflectometry: Method Extension And Comparison With Gcm Simulations

Details Four Martian Years Of Nightside Upper Thermospheric Mass Densities From Electron Reflectometry: Method Extension And Comparison With Gcm Simulations Four Martian Years Of Nightside Upper Thermospheric Mass Densities From Electron Reflectometry: Method Extension And Comparison With Gcm Simulations

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.4908l&link_type=abstract

American Astronomical Society, DPS meeting #41, #49.08

Astronomy and Astrophysics

Astronomy

Scientific paper

The long-term dynamics of the Martian upper thermosphere near the exobase ( 180 km altitude) are still relatively poorly constrained by data. Electron reflectometry (ER) provides an indirect way to infer, from the shape of electron loss cones, upper thermospheric mass densities at these altitudes in the night hemisphere, as demonstrated by our earlier work. This method requires detailed knowledge of the magnetic field in near-Mars space and thus was previously limited to 2% of the planet where 1) the permanent and predictable crustal
magnetic field dominates over the spatially and temporally variable magnetotail field and 2) where open magnetic topology allows the formation of loss cones. Here we extend the method to >50% of the planet including the northern hemisphere and compare with predictions from both the Mars Thermosphere Global Circulation Model (MTGCM) and the LMD ground-to-exosphere GCM.

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