Meteorites of Northeastern New Mexico David E
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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 -
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. -
U-Pb Age, Re-Os Isotopes, and Hse Geochemistry of Northwest Africa 6704
44th Lunar and Planetary Science Conference (2013) 1841.pdf U-PB AGE, RE-OS ISOTOPES, AND HSE GEOCHEMISTRY OF NORTHWEST AFRICA 6704. T. Iizuka1, Y. Amelin2, I. S. Puchtel3, R. J. Walker3, A. J. Irving4, A. Yamaguchi5, Y. Takagi6, T. Noguchi6 and M. Kimura5. 1Department of Earth and Planetary Science, University of Tokyo, Hongo 7-3-1, Bunkyo, Tokyo 113-0033, Japan ([email protected]), 2Research School of Earth Sciences, Australian National University, Canberra ACT, Australia, 3Department of Geology, University of Maryland, College Park, MD, USA, 4Department of Earth and Space Sciences, University of Washington, Seattle, WA, USA, 5National Institute of Polar Research, Tachikawa, Tokyo 190-8518, Japan, 6College of Science, Ibaraki University, Bunkyo 2-1-1, Mito, Ibaraki 310-8512, Japan. Introduction: Northwest Africa (NWA) 6704 is a of Maryland using standard high temperature acid diges- very unusual ungrouped fresh achondrite. It consists of tion, chemical purification and mass spectrometry tech- abundant coarse-grained (up to 1.5 mm) low-Ca py- niques [3]. The quantities of each of the HSE was at roxene, less abundant olivine, chromite, merrillite and least 1000 times greater than the blanks measured at the interstitial sodic plagioclase. Minor minerals are same time. Thus, blanks had no impact on the measure- awaruite, heazlewoodite, and pentlandite. Raman spec- ments. Accuracy and precision of Ir, Ru, Pt and Pd con- troscopy shows that a majority of the low-Ca pyroxene centrations are estimated to be <2%, of Re <0.4%, and is orthopyroxene. Bulk major element abundances are of Os <0.1%. -
Fe,Mg)S, the IRON-DOMINANT ANALOGUE of NININGERITE
1687 The Canadian Mineralogist Vol. 40, pp. 1687-1692 (2002) THE NEW MINERAL SPECIES KEILITE, (Fe,Mg)S, THE IRON-DOMINANT ANALOGUE OF NININGERITE MASAAKI SHIMIZU§ Department of Earth Sciences, Faculty of Science, Toyama University, 3190 Gofuku, Toyama 930-8555, Japan § HIDETO YOSHIDA Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan § JOSEPH A. MANDARINO 94 Moore Avenue, Toronto, Ontario M4T 1V3, and Earth Sciences Division, Royal Ontario Museum, 100 Queens’s Park, Toronto, Ontario M5S 2C6, Canada ABSTRACT Keilite, (Fe,Mg)S, is a new mineral species that occurs in several meteorites. The original description of niningerite by Keil & Snetsinger (1967) gave chemical analytical data for “niningerite” in six enstatite chondrites. In three of those six meteorites, namely Abee and Adhi-Kot type EH4 and Saint-Sauveur type EH5, the atomic ratio Fe:Mg has Fe > Mg. Thus this mineral actually represents the iron-dominant analogue of niningerite. By analogy with synthetic MgS and niningerite, keilite is cubic, with space group Fm3m, a 5.20 Å, V 140.6 Å3, Z = 4. Keilite and niningerite occur as grains up to several hundred m across. Because of the small grain-size, most of the usual physical properties could not be determined. Keilite is metallic and opaque; in reflected light, it is isotropic and gray. Point-count analyses of samples of the three meteorites by Keil (1968) gave the following amounts of keilite (in vol.%): Abee 11.2, Adhi-Kot 0.95 and Saint-Sauveur 3.4. -
Petrogenesis of Acapulcoites and Lodranites: a Shock-Melting Model
Geochimica et Cosmochimica Acta 71 (2007) 2383–2401 www.elsevier.com/locate/gca Petrogenesis of acapulcoites and lodranites: A shock-melting model Alan E. Rubin * Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90095-1567, USA Received 31 May 2006; accepted in revised form 20 February 2007; available online 23 February 2007 Abstract Acapulcoites are modeled as having formed by shock melting CR-like carbonaceous chondrite precursors; the degree of melting of some acapulcoites was low enough to allow the preservation of 3–6 vol % relict chondrules. Shock effects in aca- pulcoites include veins of metallic Fe–Ni and troilite, polycrystalline kamacite, fine-grained metal–troilite assemblages, metal- lic Cu, and irregularly shaped troilite grains within metallic Fe–Ni. While at elevated temperatures, acapulcoites experienced appreciable reduction. Because graphite is present in some acapulcoites and lodranites, it seems likely that carbon was the principal reducing agent. Reduction is responsible for the low contents of olivine Fa (4–14 mol %) and low-Ca pyroxene Fs (3–13 mol %) in the acapulcoites, the observation that, in more than two-thirds of the acapulcoites, the Fa value is lower than the Fs value (in contrast to the case for equilibrated ordinary chondrites), the low FeO/MnO ratios in acapulcoite olivine (16–18, compared to 32–38 in equilibrated H chondrites), the relatively high modal orthopyroxene/olivine ratios (e.g., 1.7 in Monument Draw compared to 0.74 in H chondrites), and reverse zoning in some mafic silicate grains. Lodranites formed in a similar manner to acapulcoites but suffered more extensive heating, loss of plagioclase, and loss of an Fe–Ni–S melt. -
Frontier Mountain Meteorite Specimens of the Acapulcoite-Lodranite Clan: Petrography, Pairing, and Parent-Rock Lithology of an Unusual Intrusive Rock
Meteoritics & Planetary Science 43, Nr 4, 731–744 (2008) Abstract available online at http://meteoritics.org Frontier Mountain meteorite specimens of the acapulcoite-lodranite clan: Petrography, pairing, and parent-rock lithology of an unusual intrusive rock Alessandro BURRONI and Luigi FOLCO* Museo Nazionale dell’Antartide, Università di Siena, Via Laterina 8, I-53100 Siena, Italy *Corresponding author. E-mail: [email protected] (Received 31 January 2007; revision accepted 10 October 2007) Abstract–In this paper we reconstruct the heterogeneous lithology of an unusual intrusive rock from the acapulcoite-lodranite (AL) parent asteroid on the basis of the petrographic analysis of 5 small (<8.3 g) meteorite specimens from the Frontier Mountain ice field (Antarctica). Although these individual specimens may not be representative of the parent-rock lithology due to their relatively large grain size, by putting together evidence from various thin sections and literature data we conclude that Frontier Mountain (FRO) 90011, FRO 93001, FRO 99030, and FRO 03001 are paired fragments of a medium- to coarse-grained igneous rock which intrudes a lodranite and entrains xenoliths. The igneous matrix is composed of enstatite (Fs13.3 ± 0.4 Wo3.1 ± 0.2), Cr-rich augite (Fs6.1 ± 0.7 Wo42.3 ± 0.9), and oligoclase (Ab80.5 ± 3.3 Or3.2 ± 0.6). The lodranitic xenoliths show a fine-grained (average grain size 488 ± 201 µm) granoblastic texture and consist of olivine Fa9.5 ± 0.4 and Fe,Ni metal and minor amounts of enstatite Fs12.7 ± 0.4 Wo1.8 ± 0.1, troilite, chromite, schreibersite, and Ca-phosphates. Crystals of the igneous matrix and lodranitic xenoliths are devoid of shock features down to the scanning electron microscope scale. -
M Iei1canjlusellm PUBLISHED by the AMERICAN MUSEUM of NATURAL HISTORY CENTRAL PARK WEST at 79TH STREET, NEW YORK 24, N.Y
jovitatesM iei1canJlusellm PUBLISHED BY THE AMERICAN MUSEUM OF NATURAL HISTORY CENTRAL PARK WEST AT 79TH STREET, NEW YORK 24, N.Y. NUMBER 2173 APRIL I4, I964 The Chainpur Meteorite BY KLAUS KEIL,1 BRIAN MASON,2 H. B. WIIK,3 AND KURT FREDRIKSSON4 INTRODUCTION This remarkable meteorite fell on May 9, 1907, at 1.30 P.M. as a shower of stones at and near the village of Chainpur (latitude 210 51' N., longi- tude 83° 29' E.) on the Ganges Plain. Some 8 kilograms were recovered. The circumstances of the fall and the recovery of the stones, and a brief description of the material, were given by Cotter (1912). One of us (Mason), when examining the Nininger Meteorite Collection in Arizona State University in January, 1962, noticed the unusual ap- pearance of a fragment of this meteorite, particularly the large chondrules and the friable texture, and obtained a sample for further investigation. Shortly thereafter, Keil was studying the Nininger Meteorite Collection, also remarked on this meteorite, and began independently to investigate it. In the meantime, Mason had sent a sample to Wiik for analysis. Under these circumstances, it seems desirable to report all these investi- gations in a single paper. 1 Ames Research Center, Moffett Field, California. 2 Chairman, Department of Mineralogy, the American Museum of Natural History. 3Research Associate, Department of Mineralogy, the American Museum of Natural History. 4Scripps Institution of Oceanography, La Jolla. 2 AMERICAN MUSEUM NOVITATES NO. 2173 FIG. 1. Photomicrograph of a thin section of the Chainpur meteorite, showing chondrules of olivine and pyroxene in a black matrix. -
History of the Institute of Meteoritics G
University of New Mexico UNM Digital Repository UNM History Essays UNM History 1988 History of the Institute of Meteoritics G. Jeffrey Taylor Follow this and additional works at: https://digitalrepository.unm.edu/unm_hx_essays Recommended Citation Taylor, G. Jeffrey. "History of the Institute of Meteoritics." (1988). https://digitalrepository.unm.edu/unm_hx_essays/12 This Article is brought to you for free and open access by the UNM History at UNM Digital Repository. It has been accepted for inclusion in UNM History Essays by an authorized administrator of UNM Digital Repository. For more information, please contact [email protected]. History of the Institute of Meteoritics G. Jeffrey Taylor The story of the Institute of Meteoritics centers on the lives of two dynamic men. One of them, Lincoln LaPaz, founded the Institute. He grew up in Kansas, where he saw Halley’s Comet at age 13 and where he gazed up at the night sky from the top of his house, studying meteors as they blazed through the atmosphere. While a student at Fairmount College in Wichita, LaPaz rode his horse, Belle, to class, letting her graze in a neighboring field while he studied mathematics. The other key figure in the Institute’s history is Klaus Keil, Director since 1968. He grew up in what became East Germany, and escaped the stifling, totalitarian life behind the iron curtain when in his young twenties, carrying meteorite specimens with him. Though having vastly different roots, LaPaz and Keil share the same fascination with stones that fall from the sky. The Institute’s story can be told in three parts: LaPaz’s era, a period of transition, and Keil’s era. -
1968 Oct 8-10 Council Minutes
Minutes of the Council Meeting of the Meteoritical Society October 8, 1968 Hoffman Geological Laboratory Harvard University Cambridge The meeting was convened at 2:15 p.m. with President Carleton B. Moore presiding. In attendance were Vice Presidents Barandon Barringer, Robert S. Dietz and John A. O'Keefe, Secretary Roy S. Clarke, Jr., Treasurer Ursula B. Marvin, Editor Dorrit Hoffleit, Past President Peter M. Millman, and Councilors Richard Barringer, Kurt Fredriksson, Gerald S. Hawkins, Klaus Keil, Brian H. Mason and John A. Wood. Robin Brett, John T. Wasson and Fred L. Whipple attended the meeting as visitors. Minutes The minutes of the Council meeting held at the Holiday Inn, Mountain View California, on October 24, 1967, were approved as submitted. Program, 31st Annual Meeting Ursula Marvin presented the program for the Annual Meeting and discussed arrangements and last minute changes. The Council unanimously approved the program as presented and thanked Mrs. Marvin and her coworkers for their efforts on behalf of the Society. Secretary's Report The report of the Secretary was submitted to the Council in writing and was accepted as submitted (copy attached). There was brief discussion of the nomenclature problem of Barringer Meteor Crater. It was pointed out that in the final analysis usage determines the name that becomes accepted. It was suggested that Society members use the name Barringer Meteor Crater in speaking and writing and that we encourage others to do the same. No other action was suggested at this time. The problem of dues for foreign members was discussed, and several individuals suggested that funds are available to help in cases of demonstrated need. -
Grove Mountains (Grv) 020043: Acapulcoite-Lodranite Genesis from the View of the Most Primitive Member
51st Lunar and Planetary Science Conference (2020) 2130.pdf GROVE MOUNTAINS (GRV) 020043: ACAPULCOITE-LODRANITE GENESIS FROM THE VIEW OF THE MOST PRIMITIVE MEMBER. T.J. McCoy1, C.M. Corrigan1, T.L. Dickinson2, G.K. Benedix3, D.L. Schrader4 and J. Davidson4, 1Dept. of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560-0119 USA ([email protected]), 2Science Matters Consulting, LLC, Washington DC 20016 USA, 3Curtin University, Bentley, WA 6102, Australia, 4Arizona State University, Tempe AZ 85287-1404 USA. Introduction: The formation of acapulcoites and An unusual, well-defined radial chondrule (Fig. 2) lodranites by partial melting of a chondritic precursor consists of a core of low- and high-Ca pyroxene rimmed has long been recognized from their broadly chondritic by SiO2 and mantled by low- and high-Ca pyroxene and mineralogy and bulk composition. Rarely, relict plagioclase. Chondrules range in diameter from ~200 to chondrules have been observed in these meteorites [1– ~2000 μm, with the mode between 400 and 500 μm and 5]. In a recent survey of acapulcoites and lodranites, [6] the mean diameter is 690 μm, essentially identical to the highlighted Grove Mountains (GRV) 020043, which results of [7]. was reclassified by [7] as a possible chondritic precursor to acapulcoites. The meteorite is remarkable for the abundance of chondrules and chondrule fragments (~62 vol.%; [7]) and mineral compositions (Fa10.7, Fs10.8) intermediate between enstatite and ordinary chondrites. [7] reported isotopic compositions for oxygen and chromium that fall within the field of acapulcoites and lodranites. Our primary motivation in studying GRV 020043 is examining several long-standing questions in acapulcoite-lodranite petrogenesis that can be uniquely addressed by such a primitive member of the group. -
Defending Planet Earth: Near-Earth Object Surveys and Hazard Mitigation Strategies Final Report
PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION Defending Planet Earth: Near-Earth Object Surveys and Hazard Mitigation Strategies Final Report Committee to Review Near-Earth Object Surveys and Hazard Mitigation Strategies Space Studies Board Aeronautics and Space Engineering Board Division on Engineering and Physical Sciences THE NATIONAL ACADEMIES PRESS Washington, D.C. www.nap.edu PREPUBLICATION COPY—SUBJECT TO FURTHER EDITORIAL CORRECTION THE NATIONAL ACADEMIES PRESS 500 Fifth Street, N.W. Washington, DC 20001 NOTICE: The project that is the subject of this report was approved by the Governing Board of the National Research Council, whose members are drawn from the councils of the National Academy of Sciences, the National Academy of Engineering, and the Institute of Medicine. The members of the committee responsible for the report were chosen for their special competences and with regard for appropriate balance. This study is based on work supported by the Contract NNH06CE15B between the National Academy of Sciences and the National Aeronautics and Space Administration. Any opinions, findings, conclusions, or recommendations expressed in this publication are those of the author(s) and do not necessarily reflect the views of the agency that provided support for the project. International Standard Book Number-13: 978-0-309-XXXXX-X International Standard Book Number-10: 0-309-XXXXX-X Copies of this report are available free of charge from: Space Studies Board National Research Council 500 Fifth Street, N.W. Washington, DC 20001 Additional copies of this report are available from the National Academies Press, 500 Fifth Street, N.W., Lockbox 285, Washington, DC 20055; (800) 624-6242 or (202) 334-3313 (in the Washington metropolitan area); Internet, http://www.nap.edu. -
Acapulcoite-Lodranite Meteorites: Ultramafic Asteroidal Partial Melt
G Model CHEMER-25432; No. of Pages 51 ARTICLE IN PRESS Chemie der Erde xxx (2017) xxx–xxx Contents lists available at ScienceDirect Chemie der Erde j ournal homepage: www.elsevier.de/chemer Invited review Acapulcoite-lodranite meteorites: Ultramafic asteroidal partial melt residues a,∗ b Klaus Keil , Timothy J. McCoy a Hawai’i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawai’i at Manoa, Honolulu, HI 96822, USA b Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560-0119, USA a r t i c l e i n f o a b s t r a c t Article history: Acapulcoites (most ancient Hf-W ages are 4,563.1 ± 0.8 Ma), lodranites (most ancient Hf-W ages are Received 13 February 2017 4,562.6 ± 0.9 Ma) and rocks transitional between them are ancient residues of different degrees of partial Received in revised form 3 April 2017 melting of a chondritic source lithology (e.g., as indicated by the occurrence of relict chondrules in 9 Accepted 21 April 2017 acapulcoites), although the precise chondrite type is unknown. Acapulcoites are relatively fine- grained ∼ ( 150–230 m) rocks with equigranular, achondritic textures and consist of olivine, orthopyroxene, Ca- Keywords: rich clinopyroxene, plagioclase, metallic Fe,Ni, troilite, chromite and phosphates. Lodranites are coarser Partial melting grained (540–700 m), with similar equigranular, recrystallized textures, mineral compositions and con- Age tents, although some are significantly depleted in eutectic Fe,Ni-FeS and plagioclase- clinopyroxene Chondritic composition Origin partial melts.