Item type |
紀要論文(ELS) / Departmental Bulletin Paper(1) |
公開日 |
2003-03-01 |
タイトル |
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タイトル |
Chemical composition of Yamato (Y) 000593 and Yamato 000749: Neutron-induced prompt gamma-ray analysis study |
言語 |
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言語 |
eng |
キーワード |
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主題Scheme |
Other |
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主題 |
Y000593 |
キーワード |
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主題Scheme |
Other |
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主題 |
Y000749 |
キーワード |
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主題Scheme |
Other |
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主題 |
prompt gamma-ray analysis (PGA) |
キーワード |
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主題Scheme |
Other |
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主題 |
chemical composition |
キーワード |
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主題Scheme |
Other |
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主題 |
hydrogen |
資源タイプ |
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資源タイプ識別子 |
http://purl.org/coar/resource_type/c_6501 |
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資源タイプ |
departmental bulletin paper |
ID登録 |
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ID登録 |
10.15094/00006027 |
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ID登録タイプ |
JaLC |
ページ属性 |
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内容記述タイプ |
Other |
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内容記述 |
P(論文) |
著者名(英) |
Oura, Yasuji
Shirai, Naoki
Ebihara, Mitsuru
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著者所属(英) |
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en |
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Department of Chemistry, Graduate School of Science, Tokyo Metropolitan University |
著者所属(英) |
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en |
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Department of Chemistry, Graduate School of Science, Tokyo Metropolitan University |
著者所属(英) |
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en |
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Department of Chemistry, Graduate School of Science, Tokyo Metropolitan University |
抄録(英) |
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内容記述タイプ |
Other |
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内容記述 |
Neutron-induced prompt gamma-ray analysis (PGA) was applied to Antarctic nakhlites, Yamato (Y) 000593 and Y000749 together with Nakhla for the non-destructive determination of most major and minor elements (plus some trace elements). In addition to analyses of lump samples of these three meteorite, powder samples representing six different portions within Y000593 also were analyzed for discussing the chemical heterogeneity. As a result, it was confirmed that most major elements are homogeneously distributed among Y000593 within an error of ±10%. Chemical compositions of Y000593 and Y000749 are essentially identical within error limits, supporting the suggestion that these meteorites are paired. Compositional similarity is also confirmed between Nakhla and Y000593 (and Y000749), verifying that Y000593 (and Y000749) belong to nakhlites. Based on our PGA data coupled with literature data for Martian meteorites, we propose a diagram used for classifying achondrites and further for grouping into individual groups of Martian meteorites. Although there are some scatterings in B and Cl data, we would propose their abundances in nakhlites to be 3.33 ppm and 80 ppm, respectively. Our H data are systematically higher than their literature data. Although further refinements in our analytical procedure of PGA are required for getting more reliable and accurate values of H in Martian meteorites, it is suspected that some literature values of H contents in Martian meteorites are a little too small. |
雑誌書誌ID |
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収録物識別子タイプ |
NCID |
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収録物識別子 |
AA11182426 |
書誌情報 |
Antarctic meteorite research
巻 16,
p. 80-93,
発行日 2003-03
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出版者 |
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出版者 |
National Institute of Polar Research |