Computer Science
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt.........4r&link_type=abstract
Thesis (PH.D.)--UNIVERSITY OF MINNESOTA, 1995.Source: Dissertation Abstracts International, Volume: 56-03, Section: B, page: 148
Computer Science
Scientific paper
A stepwise acid-etching technique has been used to examine the solar wind reservoirs of lunar and meteoritic regolith grains. Samples were treated with weak acids (rm H_2O, H_2CO_3, H_2SO_3) to facilitate the release of the most shallowly-implanted gases. Noble gas, including Kr and Xe, and nitrogen measurements of several lunar soils and one meteoritic sample are reported here. The two mineral separates measured in this study provided the most notable He and Ne results. Evidence from a previous analysis of pristine plagioclase grains from soil 60051 suggests a recent exposure to the solar wind, perhaps for the first time. Data from our plagioclase separates, however, show significant depletion of helium and neon thus precluding their use in studies of light solar wind noble gases. Light noble gas data from the two 75081 pyroxene separates are mostly consistent with previous acid etching experiments performed on pyroxene (Wieler et al., 1986; Benkert et al., 1993). Contamination problems and the possibility of incomplete recovery from the acid solution, make interpretation of nitrogen data uncertain. Acid treatments of the 79035 grain size separate however, show unambiguous evidence for the release of solar wind implanted gases. Krypton and xenon elemental data from 75081 pyroxene and a 79035 bulk size separate show these samples to retain the heavy noble gases as well as ilmenite, the mineral of choice for studies of this kind. Our data also verifies the presence in lunar fines of isotopically-heavy element ratios relative to those determined by interpolation from known solar system abundances (Cameron, 1982; Anders and Grevesse, 1989). Kr and Xe isotopic compositions for procedural steps most likely to have released recently implanted solar wind gases are consistent with the solar wind compositions proposed by Pepin et al. (1994). Their analysis suggests a krypton composition identical to the solar Kr-1 composition (Pepin, 1991) and a xenon composition that is a mixture of U-Xe and DME-Xe (Pepin and Phinney, 1978). Their analysis further suggests U-Xe and DME-Xe were separable components in the early solar system.
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