Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/112201
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dc.contributor.authorIvanova, M. A.en
dc.contributor.authorLorenz, C. A.en
dc.contributor.authorHumayun, M.en
dc.contributor.authorCorrigan, C. M.en
dc.contributor.authorLudwig, T.en
dc.contributor.authorTrieloff, M.en
dc.contributor.authorRighter, K.en
dc.contributor.authorFranchi, I. A.en
dc.contributor.authorVerchovsky, A. B.en
dc.contributor.authorKorochantseva, E. V.en
dc.contributor.authorKozlov, V. V.en
dc.contributor.authorTeplyakova, S. N.en
dc.contributor.authorKorochantsev, A. V.en
dc.contributor.authorGrokhovsky, V. I.en
dc.date.accessioned2022-05-12T08:30:22Z-
dc.date.available2022-05-12T08:30:22Z-
dc.date.issued2020-
dc.identifier.citationSierra 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.en
dc.identifier.issn1086-9379-
dc.identifier.otherAll Open Access, Bronze3
dc.identifier.urihttp://hdl.handle.net/10995/112201-
dc.description.abstractWe 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.en
dc.description.sponsorshipWe 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.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherUniversity of Arkansaen1
dc.publisherWileyen
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceMeteorit. Planet. Sci.2
dc.sourceMeteoritics and Planetary Scienceen
dc.titleSierra Gorda 009: A New Member of the Metal-Rich G Chondrites Groupleten
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/acceptedVersionen
dc.identifier.scopus85088839553-
local.contributor.employeeIvanova, M.A., Vernadsky Institute of Geochemistry and Analytical Chemistry, Moscow, 119991, Russian Federation; Lorenz, C.A., Vernadsky Institute of Geochemistry and Analytical Chemistry, Moscow, 119991, Russian Federation; Humayun, M., National High Magnetic Field Laboratory and Department of Earth, Ocean & Atmospheric Science, Florida State University, 1800 E. Paul Dirac Drive, Tallahassee, FL 32310, United States; Corrigan, C.M., National Museum of Natural History, Smithsonian Institution, Washington, District of Columbia 20560, United States; Ludwig, T., Institut für Geowissenschaften, Klaus Tschira-Labor für Kosmochemie, Ruprecht-Karls-Universität Heidelberg, Heidelberg, D-69120, Germany; Trieloff, M., Institut für Geowissenschaften, Klaus Tschira-Labor für Kosmochemie, Ruprecht-Karls-Universität Heidelberg, Heidelberg, D-69120, Germany; Righter, K., NASA – Johnston Space Center, Mailcode XI2, Houston, TX 77058, United States; Franchi, I.A., Planetary and Space Sciences Research Institute, Open University, Milton Keynes, MK7 6AA, United Kingdom; Verchovsky, A.B., Planetary and Space Sciences Research Institute, Open University, Milton Keynes, MK7 6AA, United Kingdom; Korochantseva, E.V., Vernadsky Institute of Geochemistry and Analytical Chemistry, Moscow, 119991, Russian Federation; Kozlov, V.V., Oxford Instruments OM & Gatan Inc, Moscow Office 26, Denisovskii Pereulok, Moscow, 105005, Russian Federation; Teplyakova, S.N., Vernadsky Institute of Geochemistry and Analytical Chemistry, Moscow, 119991, Russian Federation; Korochantsev, A.V., Vernadsky Institute of Geochemistry and Analytical Chemistry, Moscow, 119991, Russian Federation; Grokhovsky, V.I., Ural Federal University, Ekaterinburg, 620002, Russian Federationen
local.issue8-
local.volume55-
local.contributor.departmentVernadsky Institute of Geochemistry and Analytical Chemistry, Moscow, 119991, Russian Federation; National High Magnetic Field Laboratory and Department of Earth, Ocean & Atmospheric Science, Florida State University, 1800 E. Paul Dirac Drive, Tallahassee, FL 32310, United States; National Museum of Natural History, Smithsonian Institution, Washington, District of Columbia 20560, United States; Institut für Geowissenschaften, Klaus Tschira-Labor für Kosmochemie, Ruprecht-Karls-Universität Heidelberg, Heidelberg, D-69120, Germany; Planetary and Space Sciences Research Institute, Open University, Milton Keynes, MK7 6AA, United Kingdom; NASA – Johnston Space Center, Mailcode XI2, Houston, TX 77058, United States; Oxford Instruments OM & Gatan Inc, Moscow Office 26, Denisovskii Pereulok, Moscow, 105005, Russian Federation; Ural Federal University, Ekaterinburg, 620002, Russian Federationen
local.identifier.pure14148618-
local.description.orderMAPS13546
local.identifier.eid2-s2.0-85088839553-
local.fund.rffi20-05-00117
local.fund.feuzFEUZ-2020-0059
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