Computer Science – Learning
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p32b..03f&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P32B-03
Computer Science
Learning
[1060] Geochemistry / Planetary Geochemistry, [3662] Mineralogy And Petrology / Meteorite Mineralogy And Petrology, [6225] Planetary Sciences: Solar System Objects / Mars, [6240] Planetary Sciences: Solar System Objects / Meteorites And Tektites
Scientific paper
The ~382kg of sample returned from the lunar surface during the Apollo missions ranged from samples of gram to kilogram masses. However, any sample return mission from the martian surface will bring back small samples. Learning to get the most of each sample, while keeping enough material for future explorations, will require strategic planning and international consortium studies, as exemplified by studies of Apollo samples. Here we report on an international consortium study of 3.3 grams of olivine-phyric martian meteorite NWA 6234 as an example of what can be gleaned from a small martian sample. NWA 6234 was selected because its unusually fine grained texture suggests that it may approach a melt composition. To date, we have obtained bulk major and trace elements abundances (including highly siderophile elements; HSE), mineral compositions, Re-Os isotopes, and Li isotopes. A 100 mg slice from the interior of the sample containing an impact melt has also been scanned using high resolution X-ray computed tomography. Analyses of NWA 6234 in progress include: Ar isotopes ratios (including a separate of the impact melt vein); abundances and isotope ratios for all noble gases (for resolution of martian interior and atmosphere components using step heating); stepped combustion analyses of C and N to determine current residual and initial magmatic volatile components; melt inclusion mineralogy and chemistry to constrain original magma composition and crystallization sequence; and Sm-Nd isotope ratios to further elucidate the mantle source and age of the meteorite. So far we know that NWA 6234 has a bulk Mg# of 59 and phenocryst olivine of Fo 67. This suggests that the meteorite is more evolved than Yamato 980459 and NWA 1068. NWA 6234 has bulk REE abundances intermediate between the enriched end members (NWA 1068) and depleted (Yamato 980459) martian compositions, similar to those of basaltic shergottite Zagami. This similarity suggests another possible connection between olivine-phyric shergottites and basaltic shergottites. NWA 6234 has similar relative and absolute HSE abundances to 'normal' shergottites with >15 wt.% MgO, and a measured 187Os/188Os ratio of 0.13674±8. The δ7Li of NWA 6234 is +3.2+/- 1% and the Li concentration is 2.9 ppm, both of which fall within the range of previous measurements of martian meteorites and are consistent with a bulk inner Solar System δ7Li value. The preliminary results of our consortium, along with our ongoing work, show that much can be learned from limited sample mass; similar international and inter-laboratory collaborations will be essential for maximum science return from martian sample returns.
Abernethy F.
Butler Ian B.
Cartwright John
Chin Emily J.
Day J. M.
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