Martian atmospheric and indigenous components of xenon and nitrogen in SNC meteorites

Details Martian atmospheric and indigenous components of xenon and nitrogen in SNC meteorites Martian atmospheric and indigenous components of xenon and nitrogen in SNC meteorites

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998m%26ps...33..655m&link_type=abstract

Meteoritics & Planetary Science, vol. 33, no. 4, pp. 655-664.

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Scientific paper

In a study of the isotopic signatures of trapped xenon in shock-produced glass of shergottites and in ALH84001 we observe three components: (1) Modern Martian atmospheric Xe which is isotopically mass-fractionated relative to solar Xe, favoring the heavy isotopes, (2) solar-like Xe, as previously observed in Chassigny, (3) an isotopically fractionated (possibly ancient) component with little or no radiogenic 129Xerad. In-situ produced fission and spallation components are observed predominantly in the high-temperature steps. Heavy nitrogen signatures in ALH84001, EET79001 and Zagami reveal Martian atmospheric components. The low temperature release of ALH84001 shows evidence for the presence of a light N component ((15N ( -21e) consistent with the component observed in other SNC's. The highest observed 129Xe/130Xe ratio of 15.60 in Zagami and EET79001 is used here to represent the present Martian atmospheric component and the isotopic composition of this component is compared with other solar system Xe signatures. The 129Xe/130Xe ratios in ALH84001 are lower, but appear to reflect varying mixing ratios with other components. The consistently high 129Xe/130Xe ratios in rocks of different radiometric ages suggest that Martian atmospheric Xe evolved early on. As already concluded in earlier work, only a small fission component is observed in the Martian atmospheric component. Assuming that a chondritic 244Pu/129I initial ratio applies to Mars, this implies that either Pu-derived fission Xe is retained in the solid planet (in fact, in-situ produced fission Xe is observed in ALH84001), or may reflect a very particular degassing history of the planet.

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