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Trace element distributions in the Yamato 000593000749,NWA 817 and NWA 998 nakhlites: Implications for their petrogenesis and mantle source on Mars
https://doi.org/10.15094/00006045
https://doi.org/10.15094/0000604568259575-7a1c-43dd-bc2d-55476ff71d06
名前 / ファイル | ライセンス | アクション |
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KJ00002351413 (6.6 MB)
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Item type | 紀要論文(ELS) / Departmental Bulletin Paper(1) | |||||
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公開日 | 2004-09-01 | |||||
タイトル | ||||||
タイトル | Trace element distributions in the Yamato 000593000749,NWA 817 and NWA 998 nakhlites: Implications for their petrogenesis and mantle source on Mars | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | nakhlites | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | Mars | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | rare earth elements | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | trace elements | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | ion microprobe | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||
資源タイプ | departmental bulletin paper | |||||
ID登録 | ||||||
ID登録 | 10.15094/00006045 | |||||
ID登録タイプ | JaLC | |||||
ページ属性 | ||||||
内容記述タイプ | Other | |||||
内容記述 | P(論文) | |||||
著者名(英) |
Wadhwa, Meenakshi
× Wadhwa, Meenakshi× Crozaz, Ghislaine× Barrat, Jean-Alix |
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著者所属(英) | ||||||
en | ||||||
Department of Geology, The Field Museum | ||||||
著者所属(英) | ||||||
en | ||||||
Department of Earth and Planetary Sciences and Laboratory for Space Sciences,Washington University | ||||||
著者所属(英) | ||||||
en | ||||||
CNRS UMR 6538 (Domaines Oceaniques), U.B.O.-I.U.E.M. | ||||||
抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | We report here results of ion microprobe analyses of rare earth element abundances in various phases in the new Antarctic (paired) nakhlites Yamato 000593 and Yamato 000749, as well as in two additional nakhlites recovered from the Saharan desert, NWA 817 and NWA 998. Although these nakhlites are all composed predominantly of augite and some olivine, they differ from each other, and from the three previously known nakhlites, in the abundance and degree of crystallinity of the interstitial mesostasis. Trace element abundances in various phases in these new nakhlites indicate that they are petrogenetically related to (and comagmatic with) each other and the previously known nakhlites. The calculated parent melt compositions (in equilibrium with augite core compositions) are LREE-enriched and have REE patterns parallel to those of their whole rocks. This suggests that subsequent to accumulation of the olivine and augite, the intercumulus trapped melt evolved in a closed system. The similarity in the estimated parent melt compositions and trace element zonation in the augites of the various nakhlites indicates that these rocks are likely to have formed within a single lithologic unit on Mars. In this scenario, the differences among these nakhlites may be explained in terms of differences in the depth of crystallization within the cumulus pile, represented by different horizons within the same lithologic unit. Based on the partitioning of Eu in their augite cores, the magmatic redox conditions for the nakhlites are estimated to be relatively oxidizing (QFM), implying an oxidized source reservoir in the martian mantle. Late metasomatism of their mantle source by LREE-enriched, oxidizing fluids is suggested to be responsible for the LREE-enrichment and oxidation condition of the nakhlite parent melts. | |||||
雑誌書誌ID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA11182426 | |||||
書誌情報 |
Antarctic meteorite research 巻 17, p. 97-116, 発行日 2004-09 |
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出版者 | ||||||
出版者 | National Institute of Polar Research |