DOCSLIB.ORG

List G - Meteorites - Alphabetical List

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
List G - Meteorites - Alphabetical List LIST G - METEORITES - ALPHABETICAL LIST Specific name Group name Specific name Group name Abee Meteorite EH chondrites EETA 79001 Elephant Moraine Meteorites Acapulco Meteorite acapulcoite and shergottite acapulcoite stony meteorites Efremovka Meteorite CV chondrites Acfer Meteorites meteorites EH chondrites enstatite chondrites achondrites stony meteorites EL chondrites enstatite chondrites ALH 84001 Allan Hills Meteorites and Elephant Moraine meteorites achondrites Meteorites ALHA 77005 Allan Hills Meteorites and enstatite chondrites chondrites shergottite eucrite achondrites ALHA 77307 Allan Hills Meteorites and Fayetteville Meteorite H chondrites CO chondrites Frontier Mountain meteorites ALHA 81005 Allan Hills Meteorites and Meteorites achondrites Gibeon Meteorite octahedrite Allan Hills Meteorites meteorites GRA 95209 Graves Nunataks Meteorites Allende Meteorite CV chondrites and lodranite angrite achondrites Graves Nunataks meteorites Ashmore Meteorite H chondrites Meteorites Asuka Meteorites meteorites H chondrites ordinary chondrites ataxite iron meteorites Hammadah al Hamra meteorites aubrite achondrites Meteorites Barwell Meteorite L chondrites Haveroe Meteorite ureilite Baszkowka Meteorite L chondrites Haviland Meteorite H chondrites Belgica Meteorites meteorites HED meteorites achondrites Bencubbin Meteorite chondrites Hedjaz Meteorite L chondrites Bishunpur Meteorite LL chondrites Henbury Meteorite octahedrite Bjurbole Meteorite L chondrites hexahedrite iron meteorites Brenham Meteorite pallasite HL chondrites ordinary chondrites Bruderheim Meteorite L chondrites howardite achondrites Campo del Cielo octahedrite Indarch Meteorite EH chondrites Meteorite Innisfree Meteorite LL chondrites Canyon Diablo Meteorites octahedrite iron meteorites meteorites Cape York Meteorite iron meteorites Jilin Meteorite H chondrites carbonaceous chondrites chondrites Juvinas Meteorite eucrite CH chondrites carbonaceous chondrites K chondrites chondrites Chainpur Meteorite LL chondrites Kaba Meteorite CV chondrites chassignite SNC Meteorites Kaidun Meteorite chondrites Chassigny Meteorite chassignite Kainsaz Meteorite CO chondrites chondrites stony meteorites Kakangari Meteorite K chondrites CI chondrites carbonaceous chondrites Kapoeta Meteorite howardite CK chondrites carbonaceous chondrites Karoonda Meteorite CK chondrites CM chondrites carbonaceous chondrites Krymka Meteorite LL chondrites CO chondrites carbonaceous chondrites L chondrites ordinary chondrites Cold Bokkeveld Meteorite CM chondrites Lafayette Meteorite* meteorites Coldwater Meteorites* meteorites Leoville Meteorite CV chondrites CR chondrites carbonaceous chondrites LEW 86010 Lewis Cliff Meteorites and CV chondrites carbonaceous chondrites angrite D'Orbigny Meteorite angrite LEW 88516 Lewis Cliff Meteorites and DaG 476 Dar al Gani Meteorites and shergottite shergottite Lewis Cliff Meteorites meteorites Dar al Gani Meteorites meteorites LL chondrites ordinary chondrites Dhajala Meteorite H chondrites lodranite stony irons Dhofar Meteorites meteorites Los Angeles Meteorite shergottite diogenite achondrites Lost City Meteorite H chondrites Divnoe Meteorite stony meteorites lunar meteorites achondrites Eagle Station Meteorite pallasite MAC 88104 MacAlpine Hills Meteorites EET 87521 Elephant Moraine Meteorites and achondrites and achondrites * Does not autopost completely. 2 LIST G - METEORITES - ALPHABETICAL LIST Specific Name Group Name Specific Name Group Name MAC 88105 MacAlpine Hills Meteorites Queen Alexandra Range meteorites and achondrites Meteorites MacAlpine Hills meteorites Renazzo Meteorite CR chondrites Meteorites Rio Negro Meteorite L chondrites Malvern Meteorite howardite rumurutiites chondrites Martian meteorites achondrites Sahara Meteorites meteorites mesosiderite stony irons Saint-Severin Meteorite LL chondrites meteorites Santa Clara Meteorite iron meteorites micrometeorites meteorites SAU 005 Sayh al Uhaymir Meteorites Miller Range Meteorites meteorites and shergottite Mokoia Meteorite CV chondrites Sayh al Uhaymir meteorites Moore County Meteorite eucrite Meteorites Mundrabilla Meteorite iron meteorites Semarkona Meteorite LL chondrites Murchison Meteorite CM chondrites Sharps Meteorite H chondrites Murray Meteorite CM chondrites shergottite SNC Meteorites Nakhla Meteorite nakhlite Shergotty Meteorite shergottite nakhlite SNC Meteorites siderophyre stony irons Ningqiang Meteorite CK chondrites Sikhote-Alin Meteorite octahedrite Northwest Africa meteorites SNC Meteorites Martian meteorites Meteorites stony irons meteorites Norton County Meteorite aubrite stony meteorites meteorites octahedrite iron meteorites Tagish Lake Meteorite carbonaceous chondrites Odessa Meteorite* meteorites Tieschitz Meteorite H chondrites ordinary chondrites chondrites Toluca Meteorite octahedrite Orgueil Meteorite CI chondrites Tsarev Meteorite L chondrites pallasite stony irons ureilite achondrites Parnallee Meteorite LL chondrites Vaca Muerta Meteorite mesosiderite Pasamonte Meteorite eucrite Vigarano Meteorite CV chondrites Pecora Escarpment meteorites Warburton Meteorite ataxite Meteorites Weekeroo Station octahedrite Piplia Kalan Meteorite eucrite Meteorite Portales Valley Meteorite H chondrites Weston Meteorite H chondrites Qingzhen Meteorite EH chondrites Wolf Creek Meteorite octahedrite QUE 94201 Queen Alexandra Range Y 793605 Yamato Meteorites and Meteorites and shergottite shergottite QUE 94411 Queen Alexandra Range Yamato Meteorites meteorites Meteorites and Ybbsitz Meteorite H chondrites carbonaceous chondrites Zagami Meteorite shergottite * Does not autopost completely..
Load more

Recommended publications
  • Origin of Ureilites Inferred from a SIMS Oxygen Isotopic and Trace Element Study of Clasts in the Dar Al Gani 319 Polymict Ureilite
    Geochimica et Cosmochimica Acta, Vol. 68, No. 20, pp. 4213-4235, 2004 Copyright © 2004 Elsevier Ltd Pergamon Printed in the USA. All rights reserved 0016-7037/04 $30.00 ϩ .00 doi:10.1016/j.gca.2004.03.020 Origin of ureilites inferred from a SIMS oxygen isotopic and trace element study of clasts in the Dar al Gani 319 polymict ureilite 1,†, 2 1 1,‡ 1 3,4 NORIKO T. KITA, *YUKIO IKEDA, SHIGEKO TOGASHI, YONGZHONG LIU, YUICHI MORISHITA, and MICHAEL K. WEISBERG 1Geological Survey of Japan, AIST, AIST Central 7, Tsukuba 305-8567, Japan 2Faculty of Science, Ibaraki University, Mito 301-8512, Japan 3Department of Physical Sciences, Kingsborough College (CUNY), 2001 Oriental Boulevard, Brooklyn, NY 11235, USA 4Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024, USA (Received June 12, 2003; accepted in revised form March 3, 2004) Abstract—Secondary ion mass spectrometer (SIMS) oxygen isotope analyses were performed on 24 clasts, representing 9 clast types, in the Dar al Gani (DaG) 319 polymict ureilite with precisions better than 1‰. Olivine-rich clasts with typical ureilitic textures and mineral compositions have oxygen isotopic compositions that are identical to those of the monomict ureilites and plot along the CCAM (Carbonaceous Chondrite Anhydrous Mineral) line. Other igneous clasts, including plagioclase-bearing clasts, also plot along the CCAM line, indicating that they were derived from the ureilite parent body (UPB). Thus, we suggest that some of the plagioclase-bearing clasts in the polymict ureilites represent the “missing basaltic component” produced by partial melting on the UPB.
    [Show full text]
  • New Major and Trace Element Data from Acapulcoite-Lodranite Clan
    52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1307.pdf New Major and Trace Element Data from Acapulcoite-Lodranite Clan Meteorites: Evidence for Melt-Rock Reaction Events and Early Collisional Fragmentation of the Parent Body Michael P. Lucas1, Nick Dygert1, Nathaniel R. Miller2, and Harry Y. McSween1, 1Department of Earth & Planetary Sciences, University of Tennessee, Knoxville, [email protected], 2Department of Geological Sciences, Univer- sity of Texas at Austin. Introduction: New major and trace element data illumi- patterns exhibit negative Eu anomalies. REE patterns are nate the magmatic and thermal evolution of the acapul- generally consistent among the three groups, however coite-lodranite parent body (ALPB). We observe major comparison of calculated equilibrium melts for acapulco- and trace element disequilibrium in the acapulcoite and ite and transitional cpx and opx demonstrates disequilib- transitional groups that provide evidence for melt infil- rium partitioning in those samples, especially for light- tration and melt-rock reaction processes. In lodranites, REEs in cpx. In contrast, lodranites are in apparent trace which represent sources of the infiltrating melts, we ob- element equilibrium (Fig 1b). They are depleted in serve rapid cooling from high temperatures (hereafter REE+Y relative to acapulcoite-transitional samples in temps), consistent with collisional fragmentation of the cpx (Fig. 1a), and display consistent REE abundances parent body during differentiation. except NWA 5488, which
    [Show full text]
  • Hf–W Thermochronometry: II. Accretion and Thermal History of the Acapulcoite–Lodranite Parent Body
    Earth and Planetary Science Letters 284 (2009) 168–178 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl Hf–W thermochronometry: II. Accretion and thermal history of the acapulcoite–lodranite parent body Mathieu Touboul a,⁎, Thorsten Kleine a, Bernard Bourdon a, James A. Van Orman b, Colin Maden a, Jutta Zipfel c a Institute of Isotope Geochemistry and Mineral Resources, ETH Zurich, Clausiusstrasse 25, 8092 Zurich, Switzerland b Department of Geological Sciences, Case Western Reserve University, Cleveland, OH, USA c Forschungsinstitut und Naturmuseum Senckenberg, Frankfurt am Main, Germany article info abstract Article history: Acapulcoites and lodranites are highly metamorphosed to partially molten meteorites with mineral and bulk Received 11 November 2008 compositions similar to those of ordinary chondrites. These properties place the acapulcoites and lodranites Received in revised form 8 April 2009 between the unmelted chondrites and the differentiated meteorites and as such acapulcoites–lodranites are Accepted 9 April 2009 of special interest for understanding the initial stages of asteroid differentiation as well as the role of 26Al Available online 3 June 2009 heating in the thermal history of asteroids. To constrain the accretion timescale and thermal history of the Editor: R.W. Carlson acapulcoite–lodranite parent body, and to compare these results to the thermal histories of other meteorite parent bodies, the Hf–W system was applied to several acapulcoites and lodranites. Acapulcoites Dhofar 125 Keywords: – Δ chronology and NWA 2775 and lodranite NWA 2627 have indistinguishable Hf W ages of tCAI =5.2±0.9 Ma and Δ isochron tCAI =5.7±1.0 Ma, corresponding to absolute ages of 4563.1±0.8 Ma and 4562.6±0.9 Ma.
    [Show full text]
  • Mineralogy and Petrology of the Angrite Northwest Africa 1296 Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D
    Mineralogy and petrology of the angrite Northwest Africa 1296 Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D. Badia, C. Göpel, Marcel Bohn To cite this version: Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D. Badia, et al.. Mineralogy and petrology of the angrite Northwest Africa 1296. Meteoritics and Planetary Science, Wiley, 2005, 40 (3), pp.361-375. hal-00113853 HAL Id: hal-00113853 https://hal.archives-ouvertes.fr/hal-00113853 Submitted on 2 May 2011 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Meteoritics & Planetary Science 40, Nr 3, 361–375 (2005) Abstract available online at http://meteoritics.org Mineralogy and petrology of the angrite Northwest Africa 1296 A. JAMBON,1 J. A. BARRAT,2 O. BOUDOUMA,3 M. FONTEILLES,4 D. BADIA,1 C. GÖPEL,5 and M. BOHN6 1Laboratoire Magie, Université Pierre et Marie Curie, CNRS UMR 7047, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 2UBO-IUEM, CNRS UMR 6538, Place Nicolas Copernic, F29280 Plouzané, France 3Service du MEB, UFR des Sciences de la Terre, Université Pierre et Marie Curie, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 4Pétrologie, Modélisation des Matériaux et Processus, Université Pierre et Marie Curie, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 5Laboratoire de Géochimie et Cosmochimie, Institut de Physique du Globe, CNRS UMR 7579, 4 place Jussieu, 75252 Paris cedex 05, France 6Ifremer-Centre de Brest, CNRS-UMR 6538, BP70, 29280 Plouzané Cedex, France *Corresponding author.
    [Show full text]
  • Sulfide/Silicate Melt Partitioning During Enstatite Chondrite Melting
    61st Annual Meteoritical Society Meeting 5255.pdf SULFIDE/SILICATE MELT PARTITIONING DURING ENSTATITE CHONDRITE MELTING. C. Floss1, R. A. Fogel2, G. Crozaz1, M. Weisberg2, and M. Prinz2, 1McDonnell Center for the Space Sciences and Department of Earth and Planetary Sciences, Washington University, St. Louis MO 63130, USA ([email protected]), 2American Museum of Natural History, Department of Earth and Planetary Sciences, New York NY 10024, USA. Introduction: Aubrites are igneous rocks thought (present only in CaS-saturated charges) has a flat REE to have formed from an enstatite chondrite-like pattern with abundances of about 0.5 x CI. precursor [1]. Yet their origin remains poorly Discussion: Oldhamite/glass D values are close to understood, at least partly because of confusion over 1 for most REE, consistent with previous results the role played by sulfides, particularly oldhamite. [4,5,6], and significantly lower than those expected CaS in aubrites contains high rare earth element based on REE abundances in aubritic oldhamite. In (REE) abundances and exhibits a variety of patterns contrast, D values for FeS are surprisingly high (from [2] that reflect, to some extent, those seen in about 0.1 to 1), given the low REE abundances of oldhamite from enstatite chondrites [3]. However, natural troilite. FeS/silicate partition coefficients experimental work suggests that CaS/silicate melt reported by [5] are somewhat lower, but exhibit a REE partition coefficients are too low to account for similar pattern. Alkali loss from the charges, the high abundances observed [4,5] and do not explain resulting in Ca-enriched glass, might provide a partial the variable patterns.
    [Show full text]
  • Olivine and Pyroxene from the Mantle of Asteroid 4 Vesta ∗ Nicole G
    Earth and Planetary Science Letters 418 (2015) 126–135 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Olivine and pyroxene from the mantle of asteroid 4 Vesta ∗ Nicole G. Lunning a, , Harry Y. McSween Jr. a,1, Travis J. Tenner b,2, Noriko T. Kita b,3, Robert J. Bodnar c,4 a Department of Earth and Planetary Sciences and Planetary Geosciences Institute, University of Tennessee, Knoxville, TN 37996, USA b Department of Geosciences, University of Wisconsin, Madison, WI 53706, USA c Department of Geosciences, Virginia Tech, Blacksburg, VA 24061, USA a r t i c l e i n f o a b s t r a c t Article history: A number of meteorites contain evidence that rocky bodies formed and differentiated early in our solar Received 25 September 2014 system’s history, and similar bodies likely contributed material to form the planets. These differentiated Received in revised form 25 February 2015 rocky bodies are expected to have mantles dominated by Mg-rich olivine, but direct evidence for such Accepted 25 February 2015 mantles beyond our own planet has been elusive. Here, we identify olivine fragments (Mg# = 80–92) in Available online 17 March 2015 howardite meteorites. These Mg-rich olivine fragments do not correspond to an established lithology Editor: T. Mather in the howardite–eucrite–diogenite (HED) meteorites, which are thought to be from the asteroid 4 Keywords: Vesta; their occurrence in howardite breccias, combined with diagnostic oxygen three-isotope signatures planetary formation and minor element chemistry, indicates they are vestan.
    [Show full text]
  • Linking the Chassigny Meteorite and the Martian Surface Rock Backstay: Insights Into Igneous Crustal Differentiation Processes on Mars
    Meteoritics & Planetary Science 44, Nr 6, 853–869 (2009) Abstract available online at http://meteoritics.org Linking the Chassigny meteorite and the Martian surface rock Backstay: Insights into igneous crustal differentiation processes on Mars Hanna NEKVASIL*, Francis M. MCCUBBIN, Andrea HARRINGTON, Stephen ELARDO, and Donald H. LINDSLEY Department of Geosciences, Stony Brook University, Stony Brook, New York 11794–2100, USA *Corresponding author. E-mail: [email protected] (Received 05 August 2008; revision accepted 18 March 2009) Abstract–In order to use igneous surface lithologies to constrain Martian mantle characteristics, secondary processes that lead to compositional modification of primary mantle melts must be considered. Crystal fractionation of a mantle-derived magma at the base of the crust followed by separation and ascent of residual liquids to the surface is common in continental hotspot regions on Earth. The possibility that this process also takes place on Mars was investigated by experimentally determining whether a surface rock, specifically the hawaiite Backstay analyzed by the MER Spirit could produce a known cumulate lithology with a deep origin (namely the assemblages of the Chassigny meteorite) if trapped at the base of the Martian crust. Both the major cumulus and melt inclusion mineral assemblages of the Chassigny meteorite were produced experimentally by a liquid of Backstay composition within the pressure range 9.3 to 6.8 kbar with bulk water contents between 1.5 and 2.6 wt%. Experiments at 4.3 and 2.8 kbar did not produce the requisite assemblages. This agreement suggests that just as on Earth, Martian mantle-derived melts may rise to the surface or remain trapped at the base of the crust, fractionate, and lose their residual liquids.
    [Show full text]
  • Assessment of the Mesosiderite-Diogenite Connection and an Impact Model for the Genesis of Mesosiderites
    45th Lunar and Planetary Science Conference (2014) 2554.pdf ASSESSMENT OF THE MESOSIDERITE-DIOGENITE CONNECTION AND AN IMPACT MODEL FOR THE GENESIS OF MESOSIDERITES. T. E. Bunch1,3, A. J. Irving2,3, P. H. Schultz4, J. H. Wittke1, S. M. Ku- ehner2, J. I. Goldstein5 and P. P. Sipiera3,6 1Dept. of Geology, SESES, Northern Arizona University, Flagstaff, AZ 86011 ([email protected]), 2Dept. of Earth & Space Sciences, University of Washington, Seattle, WA, 3Planetary Studies Foundation, Galena, IL, 4Dept. of Geological Sciences, Brown University, Providence, RI, 5Dept. of Geolo- gy, University of Massachusetts, Amherts, MA, 6Field Museum of Natural History, Chicago, IL. Introduction: Among well-recognized meteorite 34) is the most abundant silicate mineral and in some classes, the mesosiderites are perhaps the most com- clasts contains inclusions of FeS, tetrataenite, merrillite plex and petrogenetically least understood. Previous and silica. Three of the ten norite clasts contain a few workers have contributed important information about tiny grains of olivine (Fa24-32). A single, fine-grained “classic” falls and Antarctic finds, and have proposed breccia clast was found in NWA 5312 (see Figure 2). several different models for mesosiderite genesis [1]. Unlike the case of pallasites, the co-occurrence of met- al and silicates (predominantly orthopyroxene and cal- cic plagioclase) in mesosiderites is inconsistent with a single-stage “igneous” history, and instead seems to demand admixture of at least two separate compo- nents. Here we review the models in light of detailed ex- amination of multiple specimens from a very large mesosiderite strewnfield in Northwest Africa. Many specimens (totaling at least 80 kilograms) from this area (probably in Algeria) have been classified sepa- rately by us and others; however, in most cases the Figure 1.
    [Show full text]
  • Thursday, August 11, 2016 EARLY SOLAR SYSTEM CHRONOLOGY I 8:30 A.M
    79th Annual Meeting of the Meteoritical Society (2016) sess701.pdf Thursday, August 11, 2016 EARLY SOLAR SYSTEM CHRONOLOGY I 8:30 a.m. Room B Chairs: Gregory Brennecka Audrey Bouvier 8:30 a.m. Kruijer T. S. * Kleine T. Tungsten Isotope Dichotomy Among Iron Meteorite Parent Bodies: Implications for the Timescales of Accretion and Core Formation [#6449] We report new combined Pt and W isotope data for IC, IIC, IIF, IIIE, and IIIF iron meteorites, with the ultimate aim of better understanding the variable pre-exposure 182W/184W signatures observed among different iron meteorite groups. 8:45 a.m. Tissot F. L. H. * Dauphas N. Grove T. L. Heterogeneity in the 238U/235U Ratios of Angrites [#6104] We report the 238U/235U ratios of six angrites. We find that the angrite-parent body was heterogeneous with regards to U isotopes. We correct the Pb-Pb ages of angrites and test their concordance with ages derived from short-lived chronometers. 9:00 a.m. Brennecka G. A. * Amelin Y. Kleine T. Combined 238U/235U and Pb Isotopics of Planetary Core Material: The Absolute Age of the IVA Iron Muonionalusta [#6296] We report a measured 238U/235U for the IVA iron Muonionalusta. This measured value requires an age correction of ~7 Myr to the previously published Pb-Pb age. This has major implications for our understanding of planetary core formation and cooling. 9:15 a.m. Cartwright J. A. * Amelin Y. Koefoed P. Wadhwa M. U-Pb Age of the Ungrouped Achondrite NWA 8486 [#6231] We report the U-Pb age for ungrouped achondrite NWA 8486 (paired with NWA 7325).
    [Show full text]
  • Physical Properties of Martian Meteorites: Porosity and Density Measurements
    Meteoritics & Planetary Science 42, Nr 12, 2043–2054 (2007) Abstract available online at http://meteoritics.org Physical properties of Martian meteorites: Porosity and density measurements Ian M. COULSON1, 2*, Martin BEECH3, and Wenshuang NIE3 1Solid Earth Studies Laboratory (SESL), Department of Geology, University of Regina, Regina, Saskatchewan S4S 0A2, Canada 2Institut für Geowissenschaften, Universität Tübingen, 72074 Tübingen, Germany 3Campion College, University of Regina, Regina, Saskatchewan S4S 0A2, Canada *Corresponding author. E-mail: [email protected] (Received 11 September 2006; revision accepted 06 June 2007) Abstract–Martian meteorites are fragments of the Martian crust. These samples represent igneous rocks, much like basalt. As such, many laboratory techniques designed for the study of Earth materials have been applied to these meteorites. Despite numerous studies of Martian meteorites, little data exists on their basic structural characteristics, such as porosity or density, information that is important in interpreting their origin, shock modification, and cosmic ray exposure history. Analysis of these meteorites provides both insight into the various lithologies present as well as the impact history of the planet’s surface. We present new data relating to the physical characteristics of twelve Martian meteorites. Porosity was determined via a combination of scanning electron microscope (SEM) imagery/image analysis and helium pycnometry, coupled with a modified Archimedean method for bulk density measurements. Our results show a range in porosity and density values and that porosity tends to increase toward the edge of the sample. Preliminary interpretation of the data demonstrates good agreement between porosity measured at 100× and 300× magnification for the shergottite group, while others exhibit more variability.
    [Show full text]
  • Formation Mechanisms of Ringwoodite: Clues from the Martian Meteorite
    Zhang et al. Earth, Planets and Space (2021) 73:165 https://doi.org/10.1186/s40623-021-01494-1 FULL PAPER Open Access Formation mechanisms of ringwoodite: clues from the Martian meteorite Northwest Africa 8705 Ting Zhang1,2, Sen Hu1, Nian Wang1,2, Yangting Lin1* , Lixin Gu1,3, Xu Tang1,3, Xinyu Zou4 and Mingming Zhang1 Abstract Ringwoodite and wadsleyite are the high-pressure polymorphs of olivine, which are common in shocked meteorites. They are the major constituent minerals in the terrestrial mantle. NWA 8705, an olivine-phyric shergottite, was heavily shocked, producing shock-induced melt veins and pockets associated with four occurrences of ringwoodite: (1) the lamellae intergrown with the host olivine adjacent to a shock-induced melt pocket; (2) polycrystalline assemblages preserving the shapes and compositions of the pre-existing olivine within a shock-induced melt vein (60 μm in width); (3) the rod-like grains coexisting with wadsleyite and clinopyroxene within a shock-induced melt vein; (4) the microlite clusters embedded in silicate glass within a very thin shock-induced melt vein (20 μm in width). The frst two occurrences of ringwoodite likely formed via solid-state transformation from olivine, supported by their mor- phological features and homogeneous compositions (Mg# 64–62) similar to the host olivine (Mg# 66–64). The third occurrence of ringwoodite might fractionally crystallize from the shock-induced melt, based on its heterogeneous and more FeO-enriched compositions (Mg# 76–51) than those of the coexisting wadsleyite (Mg# 77–67) and the host olivine (Mg# 66–64) of this meteorite. The coexistence of ringwoodite, wadsleyite, and clinopyroxene suggests a post- shock pressure of 14–16 GPa and a temperature of 1650–1750 °C.
    [Show full text]
  • An Evaluation of the Palladium-Silver Isotope Systematics in the Oldest Differentiated Planetesimal: Beyond Shock
    43rd Lunar and Planetary Science Conference (2012) 1116.pdf AN EVALUATION OF THE PALLADIUM-SILVER ISOTOPE SYSTEMATICS IN THE OLDEST DIFFERENTIATED PLANETESIMAL: BEYOND SHOCK. M.F. Horan1, R.W. Carlson1,and J. Blichert-Toft2 Department of Terrestrial Magnetism, Carnegie Institution of Washington (5241 Broad Branch Road NW, Washing- ton DC 20015. [email protected]), 2Ecole Normale Supérieure de Lyon, Université Claude Bernard Lyon 1 and CNRS (69007 Lyon, France). Introduction: Troilite from Muonionalusta (iron Troilite from slab 1 contained 5.612 ng/g Ag with meteorite group IVA) gives the oldest absolute age yet 107Ag/109Ag of 1.127±0.002, and 0.780±0.002 ng/g Pd, measured for a differentiated planetesimal corresponding to 108Pd/109Ag of 0.05946 ±0.00010. (4565.3±0.1 Ma) which suggests that the IVA parent HCl-insoluble inclusions (probably schreibersite) with- body accreted, differentiated, and cooled within 2-3 in this troilite yielded 1.758±0.006 ng/g Ag with Ma after CAI formation [1]. The aim of this study is to 107Ag/109Ag of 1.130±0.002, and 5168±10 ng/g Pd, use the quick evolution and volatile-depleted (high corresponding to 108Pd/109Ag of 1691±8. Troilite from Pd/Ag) composition of IVA irons to better constrain slab 2 contained 11.75±0.04 ng/g Ag and had a the initial Solar System abundance of 107Pd ( 107Pd 107Ag/109Ag ratio of 1.0833±0.0004 [6]. The Pd con- 107 Ag with t1/2 = 6.5 Ma). Most Pd/Ag ages have been centration was 0.291±0.1 ng/g corresponding to referenced to 107Pd/108Pd = (2.40±0.05) x 10-5 obtained 108Pd/109Ag of 13.9±0.1.
    [Show full text]