Fractionated martian atmosphere in the nakhlites?

Details Fractionated martian atmosphere in the nakhlites? Fractionated martian atmosphere in the nakhlites?

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994metic..29..854d&link_type=abstract

Meteoritics (ISSN 0026-1114), vol. 29, no. 6, p. 854-859

Computer Science

40

Chemical Fractionation, Isotopes, Mars Atmosphere, Meteoritic Composition, Nakhlites, Rare Gases, Crystallization, Leaching, Olivine, Sediments, Temperature Effects

Scientific paper

Considerable evidence points to a martian origin of the shergottite-nakhlite-chassignite (SNC) meteorites. Noble gas isotopic compositions have been measured in most SNC meteorites. The Xe-129/Xe-132 vs. Kr-84/Xe-132 ratios in Chassigny, most shergottites, and lithology C of EETA 79001 define a linear array. This array is thought to be a mixing line between martian mantle and martian atmosphere. One of the SNC meteorites, Nakhla, contains a leachable component that has an elevated Xe-129/Xe-132 ratio relative to its Kr-84/Xe-132 ratio when compared to this approximately linear array. 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 elevated Xe isotopic ratio may represent a distinct reservoir in the martian crust or mantle. More plausibly, it is elementally fractionated martian atmosphere. Formation of sediments fractionates the noble gases in the correct direction. The range of sediment/atmosphere fractionation factors is consistent with the elevated Xe-129/Xe-132 component in Nakhla being contained in iddingsite, a low temperature weathering product. The crystallization age of Nakhla is 1.3 Ga. Its low-shock state suggests that it was ejected from near the surface of Mars. As liquid water is required for the formation of iddingsite, these observations provide further evidence for the near surface existence of aqueous fluids on Mars more recently than 1.3 Ga.

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