Biology
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p13a1655s&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P13A-1655
Biology
[0343] Atmospheric Composition And Structure / Planetary Atmospheres, [5210] Planetary Sciences: Astrobiology / Planetary Atmospheres, Clouds, And Hazes, [5405] Planetary Sciences: Solid Surface Planets / Atmospheres, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
In 2008, NASA's Mars Phoenix Lander measured perchlorate (salts containing ClO4-) concentrations of 0.6 wt%; an amount that is larger than the highest natural concentrations found on Earth [1,2]. However, the origin of Martian perchlorate is unknown. Perchlorates are interesting because some forms are highly deliquescent with very low eutectic temperatures, allowing the possibility of liquids on Mars today. Also, if perchlorates formed via photochemistry (as on Earth), potentially they can be used as a tracer of the past chemistry of the Martian atmosphere. On Earth, naturally-occurring perchlorate is found only in extremely arid areas, such as deserts or within stratospheric aerosols. Recently, [2] modeled the formation of perchlorate over the driest place on Earth, the Atacama Desert. In this mechanism, natural emissions of chlorine-containing volatiles (e.g. HCl) react with photochemically-produced oxidants to make perchloric acid, HClO4. The acid is then dry deposited onto the surface where it forms perchlorate salts. A similar process could have occurred on Mars when the planet was volcanically active. Here, we add halogen and sulfur chemistry to a Martian photochemical model [3] in order to study an analogous formation mechanism for perchlorate on Mars. The model applies for the period over which Mars was volcanically active and dry, as was the case during much of the Hesperian and Amazonian eras. The model boundary conditions include the deposition velocities of halogen species onto the surface, the odd-nitrogen flux from the ionosphere, and the composition of volcanic gases. Varying the boundary conditions tests the model sensitivity. Surface depositional fluxes for perchlorates, and also nitrates and sulfates, are calculated. Model results are then compared to observations of salts on the surface, providing insight into Martian surface mineralogy.
Catling David C.
Claire Mark
Smith Marcie
Zahnle Kevin J.
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