Atmosphere-surface interactions and atmospheric evolution on Mars

Details Atmosphere-surface interactions and atmospheric evolution on Mars Atmosphere-surface interactions and atmospheric evolution on Mars

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992msat.work...49f&link_type=abstract

In Lunar and Planetary Inst., Workshop on the Martian Surface and Atmosphere Through Time p 49-50 (SEE N92-28988 19-91)

Other

Air Land Interactions, Atmospheric Composition, Losses, Mars Atmosphere, Outgassing, Planetary Evolution, Volatility, Carbon Dioxide, Nitrogen, Temperature Profiles, Water

Scientific paper

A knowledge of the original volatile endowment of Mars is essential for any discussion of atmospheric loss on this planet. Cosmochemical models which postulate that planetary bulk compositions and volatile contents were controlled by the radial temperature profile in the solar nebula, and estimated bulk compositions based on the assumption that Mars is the parent body for the SNC meteorites predicts that Mars is volatile-rich. However, contrary views can also be found. For illustrative purposes, it is assumed that Mars was volatile-rich initially like the Earth. Taking terrestrial volatiles as the sum of the atmospheric, crustal, and oceanic volatiles and assuming that Mars accreted with the same volatile content on a g/g basis, the volatile endowments for an Earth-like Mars correspond to approximately 14 bars CO2, 800 mbars N2, and 1.2 km H2O. Subsequent topics discussed are: composition of outgassing volatiles; rates of present day atmospheric-surface reactions; constraints on CO2 loss via carbonate formation; constraints on H2O loss; and loss of other volatiles.

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