HDO in the Martian atmosphere - Implications for the abundance of crustal water

Details HDO in the Martian atmosphere - Implications for the abundance of crustal water HDO in the Martian atmosphere - Implications for the abundance of crustal water

Oct 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988icar...76..146y&link_type=abstract

Icarus (ISSN 0019-1035), vol. 76, Oct. 1988, p. 146-159.

Mathematics

Logic

69

Abundance, Atmospheric Models, Heavy Water, Mars Atmosphere, Planetary Composition, Planetary Crusts, Air Water Interactions, Geomorphology, Photochemical Reactions, Surface Water

Scientific paper

A one-dimensional photochemical model is presently used to ascertain the nature of those chemical and physical processes of the Martian atmosphere responsible for the preferential escape of hydrogen over deuterium. A comparison of the present theoretical considerations with recent HDO observations indicates that Mars contains 0.2 m of (globally averaged) crustal water that is exchangeable with the atmosphere. This estimate, which is substantially lower than those obtained for Martian subsurface water on the basis of Viking image-derived geomorphological analyses, can be reconciled only if a small fration of the crustal water is exchangeable with the atmosphere.

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