Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.4905d&link_type=abstract
American Astronomical Society, DPS meeting #41, #49.05
Astronomy and Astrophysics
Astronomy
Scientific paper
When modeling thick, early Martian atmospheres to find atmospheric loss rates and surface UV conditions, it is often assumed that the column integrated ratios of CO2, O2, CO, and O3 were the same as those observed today. Even when photochemical models are used to determine the composition of past atmospheres, a temperature profile similar to that currently observed is often imposed as a simplification. However, neither of these may be accurate assumptions. With a thicker CO2 atmosphere, a significant O3 layer could potentially form, heating the middle atmosphere and altering the temperature profile. Equilibrium levels of O2 and CO would also be expected to change. With a decreased UV flux in the lower atmosphere, the H2O photolysis rate would be reduced, and if higher O2 levels were present the temperature of the Martian thermosphere would be elevated. These changes have implications for the loss of species to space, as well as the clemency of the Martian surface for primitive life, and a potential resolution to the Faint-Sun Paradox. Preliminary examination of this concept with a 1D radiative-convective model and a basic photochemical model are presented.
Deighan Justin
Johnson Robert E.
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