The Sources of Water in Martian Meteorites

Details The Sources of Water in Martian Meteorites The Sources of Water in Martian Meteorites

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusm.p41a..11b&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #P41A-11

Physics

6225 Mars

Scientific paper

H isotope measurements of carbonate, phosphate, feldspathic and mafic glasses, and post-stishovite silica phase in the shergottites Zagami, Shergotty, SaU 005, DaG 476, ALHA 77005 and EETA 79001 and in Chassigny and ALH 84001 show that they contain a D-enriched component of extraterrestrial origin. Although the minerals and glasses analyzed seem to contain an initial primary H component, their isotopic composition was modified to varying degrees by three different processes: interaction with a fractionated exchangeable water reservoir on Mars, hydrogen devolatilization by impact melting, and terrestrial contamination. Positive correlation between \deltaD and water abundance in feldspathic glass and post-stishovite silica in Zagami, Shergotty, and SaU 005 is indicative of mixing of a high \deltaD component (3000 - 4000\permil) and a low \deltaD (\0permil) "magmatic" component. The negative correlation between \deltaD and water abundances in mafic and feldspathic glasses in ALH 84001, ALHA 77005, and EETA 79001 is consistent with addition of a low \deltaD terrestrial contaminant to a high D Martian component. The low \deltaD of magmatic glass in melt inclusions suggests that \deltaD of Martian parent magma is low and that the initial H isotope signature of Mars may be similar to that of earth.

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