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Earth and Planetary Science Letters 353–354 (2012) 208–218 Contents lists available at SciVerse ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl Rhenium–osmium isotope and highly-siderophile-element abundance systematics of angrite meteorites Amy J.V. Riches a,n, James M.D. Day b,c, Richard J. Walker c, Antonio Simonetti d, Yang Liu a, Clive R. Neal d, Lawrence A. Taylor a a Planetary Geosciences Institute, Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37966, United States b Geosciences Research Division, Scripps Institution of Oceanography, La Jolla, CA 92093-0244, United States c Department of Geology, University of Maryland, College Park, MD 20742, United States d Department of Civil and Environmental Engineering and Earth Sciences, 156 Fitzpatrick Hall, University of Notre Dame, Notre Dame, IN 46556, United States article info abstract Article history: Coupled 187Os/188Os compositions and highly-siderophile-element (HSE: Os, Ir, Ru, Pt, Pd, and Re) Received 24 February 2012 abundance data are reported for eight angrite achondrite meteorites that include quenched- and Received in revised form slowly-cooled textural types. These data are combined with new major- and trace-element concentra- 17 July 2012 tions determined for bulk-rock powder fractions and constituent mineral phases, to assess angrite Accepted 8 August 2012 petrogenesis. Angrite meteorites span a wide-range of HSE abundances from 0.005 ppb Os (e.g., Editor: T. Elliott o Available online 15 September 2012 Northwest Africa [NWA] 1296; Angra dos Reis) to 4100 ppb Os (NWA 4931). Chondritic to supra- chondritic 187Os/188Os (0.1201–0.2127) measured for Angra dos Reis and quenched-angrites corre- Keywords: spond to inter- and intra-sample heterogeneities in Re/Os and HSE abundances. Quenched-angrites angrites have chondritic-relative rare-earth-element (REE) abundances at 10–15 Â CI-chondrite, and their Os- osmium isotopes isotope and HSE abundance variations represent mixtures of pristine uncontaminated crustal materials highly-siderophile-elements planetary differentiation that experienced addition (o0.8%) of exogenous chondritic materials during or after crystallization. impact processes Slowly-cooled angrites (NWA 4590 and NWA 4801) have fractionated REE-patterns, chondritic to sub- 187 188 late accretion chondritic Os/ Os (0.1056–0.1195), as well as low-Re/Os (0.03–0.13), Pd/Os (0.071–0.946), and relatively low-Pt/Os (0.792–2.640). Sub-chondritic 187Os/188Os compositions in NWA 4590 and NWA 4801 are unusual amongst planetary basalts, and their HSE and REE characteristics may be linked to melting of mantle sources that witnessed prior basaltic melt depletion. Angrite HSE-Yb systematics suggest that the HSE behaved moderately-incompatibly during angrite magma crystallization, implying the presence of metal in the crystallizing assemblage. The new HSE abundance and 187Os/188Os compositions indicate that the silicate mantle of the angrite parent body(ies) (APB) had HSE abundances in chondritic-relative proportions but at variable abundances at the time of angrite crystallization. The HSE systematics of angrites are consistent with protracted post-core formation accretion of materials with chondritic-relative abundances of HSE to the APB, and these accreted materials were rapidly, yet inefficiently, mixed into angrite magma source regions early in Solar System history. & 2012 Elsevier B.V. All rights reserved. 1. Introduction 53Mn-53Cr, 26Al-26Mg and 182Hf-182W systematics, show that angrites are some of the most ancient differentiated Solar System Angrites are broadly basaltic achondrite meteorites that crys- materials, with ages of 4564–4568 Ma (e.g., Amelin, 2008, Amelin tallized from magmas generated within an early-formed differ- et al., 2009; Baker et al., 2005; Connelly et al., 2008; Kleine et al., entiated parent body(ies), within 2–10 Myrs of the formation of 2012; Lugmair and Galer, 1992; Nyquist et al., 2009). The calcium aluminum-rich inclusions (CAIs; e.g., Kleine et al., 2009; relatively homogeneous D17O compositions (D17O¼0.0727 Markowski et al., 2007; Quitte´ et al., 2010). Absolute U-Pb 0.007% (1s); D17O defined in the supplementary materials) that chronology, coupled with relative-age chronometry from differ from terrestrial (D17O¼0%), lunar (0%), martian (þ0.3%), and howardite–eucrite–diogenite (HED; D17O¼0.23%)compo- sitions, indicate that angrites were derived from one or more distinct n Correspondence to: University of Alberta, Department of Earth and angrite parent bodies (APB), which experienced large-scale melting, Atmospheric Sciences, 1-26 Earth Sciences Building, Edmonton, Alberta, Canada T6G 2E3. Tel.: þ1 780 492 2676; fax: þ1 780 492 2030. differentiation, and O-isotopic homogenization (Clayton, 2003; E-mail address: [email protected] (A.J.V. Riches). Franchi, 2008; Greenwood et al., 2005; Mittlefehldt et al., 2008). 0012-821X/$ - see front matter & 2012 Elsevier B.V. All rights reserved. http://dx.doi.org/10.1016/j.epsl.2012.08.006 Table 1 Highly-siderophile-element abundances (ppb) and osmium isotope data for angrite meteorites. Sample Group Mass (g) Os Blk (%) Ir Blk (%) Ru Blk (%) Pt Blk (%) Pd Blk (%) Re Blk (%)Ren 72r 187Re/188Os 72r 187Ren/188Os Angra Dos Reis Slowly-cooled Ra 0.191 0.0045 44.3 0.027 9 0.008 46 0.173 23 0.022 79 0.0014 99 0.0014 0.0007 1.49 1.08 1.475 M 0.239 0.096 4.6 0.053 18 0.267 7 0.537 2 0.041 38 0.0148b 95 0.0088 0.0005 0.74 0.95 0.440 D’Orbigny Quenched R 0.286 2.481 0.10 6.036 0.1 6.411 0.1 5.251 0.6 3.729 2 0.588 0.8 0.1558 0.0006 1.14 0.01 0.302 Ma 0.525 0.077 2.7 0.055 29 0.164 6 0.265 2 0.607 5 0.015 10 0.0168 0.0005 0.93 0.10 1.052 Sahara 99555 Quenched R 0.265 0.240 1.06 0.249 2 0.547 1 0.937 4 0.420 4 0.050c 10 0.0385 0.0006 1.01 0.10 0.776 Ma 0.896 0.121 1.02 0.137 21 0.203 3 0.458 0.6 0.504 3 0.025b 4 0.0290 0.0003 1.01 0.04 1.164 A881371, 55 Quenched M 0.194 0.307 0.37 0.288 2 0.315 12 0.801 4.4 0.239 46 0.039 10 0.0315 0.0003 0.61 0.10 0.496 A.J.V. Riches et al. / Earth and Planetary Science Letters 353–354 (2012) 208–218 NWA 1296 Quenched M 0.304 0.0056 6.49 0.0088 13 0.0247 36 0.0110 67 0.0039 71 0.0008 64 0.0008 0.0001 0.66 0.64 0.718 NWA 4590 Slowly-cooled Ra 0.297 2.66 0.09 4.44 0.1 7.32 0.06 5.90 0.6 1.52 4 0.152 3 0.1577 0.0006 0.28 0.03 0.286 Ma 0.503 1.89 0.12 3.25 1 4.94 0.2 4.99 0.1 1.79 2 0.238b 0.4 0.1157 0.0005 0.61 0.01 0.295 NWA 4801 Slowly-cooled Ra 0.314 14.16 0.005 15.0 0.03 28.4 0.01 12.4 0.3 1.68 3 0.379 0.5 0.349 0.002 0.128 0.007 0.119 Ma 0.448 10.47 0.024 10.07 0.4 9.20 0.1 8.28 0.1 0.74 5 0.279 0.4 0.297 0.004 0.128 0.006 0.136 NWA 4931 Anomalous R 0.313 135 0.002 – – – – – – – – – – 11.43 0.02 – – 0.409 M 0.310 114.9 0.003 133.36 0.03 216.04 0.01 243.55 0.004 173.40 0.03 9.08 0.02 9.99 0.02 0.381 0.005 0.419 M 0.353 97.22 0.080 107.07 0.02 178.14 0.04 207.07 0.02 146.41 0.01 8.78 0.03 8.23 0.09 0.435 0.005 0.408 187 188 187 188 n Sample Os/ Os 72r Os/ Osi 72rcOsi 72r Re/Os Re /Os Pt/Os Os/Ir (Pt/Pd)N (Pd/Os)N Angra Dos Reis Rn 0.2127 0.0062 0.095 0.121 À1.1 2.7 0.31 0.31 38.56 0.168 5.096 4.001 M 0.13094 0.00035 0.072 0.106 À24.8 1.3 0.15 0.09 5.583 1.819 8.621 0.342 D’Orbigny R 0.12007 0.00007 0.030 0.002 À68.9 2.0 0.24 0.06 2.117 0.411 0.924 1.212 Mn 0.17927 0.00022 0.106 0.012 9.8 1.7 0.19 0.22 3.429 1.398 0.287 6.315 Sahara 99555 R 0.15745 0.00020 0.077 0.012 À19.5 1.8 0.21 0.16 3.906 0.962 1.464 1.411 Mn 0.18813 0.00013 0.109 0.005 13.0 1.8 0.21 0.24 3.792 0.882 0.596 3.363 A881371. 55 M 0.13538 0.00019 0.087 0.011 À9.7 1.1 0.13 0.10 2.614 1.064 2.197 0.629 NWA 1296 M 0.15287 0.00050 0.101 0.072 4.5 1.2 0.14 0.14 1.967 0.638 1.865 0.558 NWA 4590 Rn 0.11876 0.00006 0.097 0.003 0.8 0.5 0.06 0.06 2.222 0.598 2.553 0.460 Mn 0.11947 0.00007 0.072 0.001 À25.6 1.1 0.13 0.06 2.640 0.582 1.830 0.763 NWA 4801 Rn 0.10556 0.00006 0.095 0.001 À0.8 0.2 0.03 0.02 0.873 0.945 4.825 0.096 Mn 0.10696 0.00015 0.097 0.001 0.7 0.2 0.03 0.03 0.792 1.040 7.306 0.057 NWA 4931 R 0.12852 0.00005 – – – – – 0.08 – – – – M 0.12927 0.00006 0.099 0.001 3.1 0.7 0.08 0.09 2.119 0.862 0.921 1.216 M 0.12839 0.00030 0.094 0.001 À2.3 0.8 0.09 0.08 2.130 0.908 0.928 1.214 The uncertainty (%) associated with each abundance measurement reflects the propagated blank correction (Blk) derived from the measured blank of the corresponding analytical cohort.
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    geosciences Review Reviewing Martian Atmospheric Noble Gas Measurements: From Martian Meteorites to Mars Missions Thomas Smith 1,* , P. M. Ranjith 1, Huaiyu He 1,2,3,* and Rixiang Zhu 1,2,3 1 State Key Laboratory of Lithospheric Evolution, Institute of Geology and Geophysics, Chinese Academy of Sciences, 19 Beitucheng Western Road, Box 9825, Beijing 100029, China; [email protected] (P.M.R.); [email protected] (R.Z.) 2 Institutions of Earth Science, Chinese Academy of Sciences, Beijing 100029, China 3 College of Earth and Planetary Sciences, University of Chinese Academy of Sciences, Beijing 100049, China * Correspondence: [email protected] (T.S.); [email protected] (H.H.) Received: 10 September 2020; Accepted: 4 November 2020; Published: 6 November 2020 Abstract: Martian meteorites are the only samples from Mars available for extensive studies in laboratories on Earth. Among the various unresolved science questions, the question of the Martian atmospheric composition, distribution, and evolution over geological time still is of high concern for the scientific community. Recent successful space missions to Mars have particularly strengthened our understanding of the loss of the primary Martian atmosphere. Noble gases are commonly used in geochemistry and cosmochemistry as tools to better unravel the properties or exchange mechanisms associated with different isotopic reservoirs in the Earth or in different planetary bodies. The relatively low abundance and chemical inertness of noble gases enable their distributions and, consequently, transfer mechanisms to be determined. In this review, we first summarize the various in situ and laboratory techniques on Mars and in Martian meteorites, respectively, for measuring noble gas abundances and isotopic ratios.
  • Trace Element Chemistry of Cumulus Ridge 04071 Pallasite with Implications for Main Group Pallasites

    Trace Element Chemistry of Cumulus Ridge 04071 Pallasite with Implications for Main Group Pallasites

    Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites Item Type Article; text Authors Danielson, L. R.; Righter, K.; Humayun, M. Citation Danielson, L. R., Righter, K., & Humayun, M. (2009). Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites. Meteoritics & Planetary Science, 44(7), 1019-1032. DOI 10.1111/j.1945-5100.2009.tb00785.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 23/09/2021 14:17:54 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656592 Meteoritics & Planetary Science 44, Nr 7, 1019–1032 (2009) Abstract available online at http://meteoritics.org Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites Lisa R. DANIELSON1*, Kevin RIGHTER2, and Munir HUMAYUN3 1Mailcode JE23, NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas 77058, USA 2Mailcode KT, NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas 77058, USA 3National High Magnetic Field Laboratory and Department of Geological Sciences, Florida State University, Tallahassee, Florida 32310, USA *Corresponding author. E-mail: [email protected] (Received 06 November 2008; revision accepted 11 May 2009) Abstract–Pallasites have long been thought to represent samples from the metallic core–silicate mantle boundary of a small asteroid-sized body, with as many as ten different parent bodies recognized recently. This report focuses on the description, classification, and petrogenetic history of pallasite Cumulus Ridge (CMS) 04071 using electron microscopy and laser ablation ICP-MS.