The Martian surface radiation environment - Influence of higher atmospheric pressure and surface or sub-surface water

Details The Martian surface radiation environment - Influence of higher atmospheric pressure and surface or sub-surface water The Martian surface radiation environment - Influence of higher atmospheric pressure and surface or sub-surface water

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p21a1640e&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P21A-1640

Physics

[5405] Planetary Sciences: Solid Surface Planets / Atmospheres, [5421] Planetary Sciences: Solid Surface Planets / Interactions With Particles And Fields, [6225] Planetary Sciences: Solar System Objects / Mars

Scientific paper

The Noachian epoch (~4.5 - 3.5 billion years ago) is a promising era for a possible emergence of life on Mars. The presence of runoff channels in areas formed during the Noachian suggests that liquid water existed at least sporadically during that time, with liquid water being regarded as a prerequisite for life. To have sustained liquid water, the atmospheric pressure on Noachian Mars must have been significantly higher than in the present. When considering the possibility of life on Noachian Mars, one conceivable restriction is given by the ionizing radiation environment. Using PLANETOCOSMICS- and GEANT4-simulation codes, we calculate the radiation environment on the Martian surface and the resulting radiation exposure for different atmospheric conditions. Here, we present absorbed dose rates resulting from galactic-cosmic-proton and alpha-particle-induced radiation environments, as well as changes of these rates caused by an increase of atmospheric pressure. Furthermore, we analyze which influence the presence of liquid surface water or sub-surface water-ice would have on the radiation environment under these different atmospheric conditions.

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