Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.2401v&link_type=abstract
American Astronomical Society, DPS meeting #39, #24.01; Bulletin of the American Astronomical Society, Vol. 39, p.454
Astronomy and Astrophysics
Astronomy
Scientific paper
As a part of a global effort, the dynamics of the flow of energetic particles through the Martian upper atmosphere has been studied. Being the most important reaction, the dissociative recombination (DR) of O2+ is responsible of most of the production of hot atomic oxygen deep in the thermosphere of Mars. To understand the Martian exosphere, it is then necessary to employ a global kinetic model that can include a self-consistent description of both thermosphere collisional region and exospheric collisionless domain.
In this study, we have used our Direct Simulation Monte Carlo (DSMC) model in combination with the 3D Mars Thermosphere General Circulation Model (MTGCM) of Bougher et al. [2006, Geophys. Res. Lett., 33, doi:10.1029/2005GL024059.] to describe self-consistently the region of the upper thermosphere where the exosphere is generated, the entire exosphere, and its feedback into the thermosphere generally. Along with the effect of ionization, the DSMC method allows us to provide profiles of density and temperature, atmospheric loss rates and return fluxes as functions of the Solar Zenith Angle (SZA) for all cases considered.
To present a complete description of this physical problem we examined several of the most limiting cases spanning spatial and temporal domains. Along with solar activity variability, these include comparisons between the polar meridian and the equator at equinox and between the summer and winter polar meridians at perihelion and aphelion conditions, respectively.
Support for this work comes from NASA Mars Fundamental Research grant NNG05GL80G.
Bougher Stephen W.
Combi Michael R.
Nagy Andrew F.
Tenishev Valeriy
Valeille Arnaud
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