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Title: Sierra Gorda 009: A New Member of the Metal-Rich G Chondrites Grouplet
Authors: Ivanova, M. A.
Lorenz, C. A.
Humayun, M.
Corrigan, C. M.
Ludwig, T.
Trieloff, M.
Righter, K.
Franchi, I. A.
Verchovsky, A. B.
Korochantseva, E. V.
Kozlov, V. V.
Teplyakova, S. N.
Korochantsev, A. V.
Grokhovsky, V. I.
Issue Date: 2020
Publisher: University of Arkansa
Citation: Sierra Gorda 009: A New Member of the Metal-Rich G Chondrites Grouplet / M. A. Ivanova, C. A. Lorenz, M. Humayun et al. // Meteoritics and Planetary Science. — 2020. — Vol. 55. — Iss. 8. — MAPS13546.
Abstract: We investigated the metal-rich chondrite Sierra Gorda (SG) 009, a member of the new G chondrite grouplet (also including NWA 5492, GRO 95551). G chondrites contain 23% metal, very reduced silicates, and rare oxidized mineral phases (Mg-chromite, FeO-rich pyroxene). G chondrites are not related to CH-CB chondrites, based on bulk O, C, and N isotopic compositions, mineralogy, and geochemistry. G chondrites have no fine-grained matrix or matrix lumps enclosing hydrated material typical for CH-CB chondrites. G chondrites’ average metal compositions are similar to H chondrites. Siderophile and lithophile geochemistry indicates sulfidization and fractionation of the SG 009 metal and silicates, unlike NWA 5492 and GRO 95551. The G chondrites have average O isotopic compositions Δ17O'0‰ ranging between bulk enstatite (E) and ordinary (O) chondrites. An Al-rich chondrule from SG 009 has Δ17O'0‰ indicating some heterogeneity in oxygen isotopic composition of G chondrite components. SG 009’s bulk carbon and nitrogen isotopic compositions correspond to E and O chondrites. Neon isotopic composition reflects a mixture of cosmogenic and solar components, and cosmic ray exposure age of SG 009 is typical for O, E, and R chondrites. G chondrites are closely related to O, E, and R chondrites and may represent a unique metal-rich parent asteroid containing primitive and fractionated material from the inner solar system. Oxidizing and reducing conditions during SG 009 formation may be connected with a chemical microenvironment and possibly could indicate that G chondrites may have formed by a planetesimal collision resulting in the lack of matrix. © The Meteoritical Society, 2020.
Access: info:eu-repo/semantics/openAccess
SCOPUS ID: 85088839553
PURE ID: 14148618
ISSN: 1086-9379
metadata.dc.description.sponsorship: We thank M. Weisberg, H. Downes, an anonymous reviewer, and Associate Editor C. Goodrich, for their thoughtful reviews which helped to improve this paper. The authors thank Sasha Krot for very fruitful discussions. This work was supported by the Russian Fond of Basic Research no. 20-05-00117A, by Klaus Tschira Stiftung gGmbH, by the NASA Emerging Worlds program (80NSSC18K0595, MH), and we thank the National High Magnetic Field Laboratory, which is supported by National Science Foundation Cooperative Agreement No. DMR-1644779* and the State of Florida. This work was also supported?by the Project No. FEUZ-2020-0059 of the Ministry of Science and Higher Education of the Russian Federation. This study was a partial contribution to research theme no. 0137-2019-0002.
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