Noble gas evidence of an aqueous reservoir near the surface of Mars more recently than 1.3 GA

Details Noble gas evidence of an aqueous reservoir near the surface of Mars more recently than 1.3 GA Noble gas evidence of an aqueous reservoir near the surface of Mars more recently than 1.3 GA

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24..431d&link_type=abstract

In Lunar and Planetary Inst., Twenty-fourth Lunar and Planetary Science Conference. Part 1: A-F p 431-432 (SEE N94-12015 01-91)

Computer Science

Igneous Rocks, Lithology, Mars Atmosphere, Mars Surface, Planetary Crusts, Planetary Mantles, Planetary Structure, Rare Gases, Shergottites, Water, Crystallization, Mars (Planet), Olivine, Planetary Geology, Radiogenic Materials, Sediments, Silicates

Scientific paper

Considerable evidence points to a Martian origin of the SNC meteorites. One of these meteorites, Nakhla, contains a leachable component which has an elevated Xe-129/Xe-132 ratio relative to its Kr-84/Xe-132 ratio when compared to the approximately linear array defined by Chassigny, most shergottites, and lithology C of EETA 79001. This array is thought to be a mixing line between Martian mantle and Martian atmosphere. The leachable component probably consists in part of iddingsite, an alteration product produced by interaction of olivine with aqueous fluid at temperatures lower than 150 C. The radiogenic Xe component may represent a distinct reservoir in the Martian crust or mantle. More plausibly, it is Martian atmosphere, fractionated by solution in liquid water and by interaction with sediment. The crystallization age of Nakhla is 1.3 Ga. Its low shock state suggests that it was ejected from near the surface of Mars. Liquid water is required for the formation of iddingsite. These observations provide further evidence for the near surface existence of aqueous fluids more recently than 1.3 Ga.

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