DOCSLIB.ORG

The Alexandre DEBIENNE Météorite Collection Update : Sept

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Alien Rocks The Alexandre DEBIENNE Météorite Collection Update : Sept. 2015. NOM LOCALISATION TYPE TYPE2 Shape POIDS/gr Abu Moharek Egypte Chondrite olivine bronzite H H4 Slice 15.00gr Acfer 344 Aldérie Chondrite olivine bronzite H H3 Slice 4.10gr Acfer 358 Aldérie Chondrite olivine bronzite H H6 Slice 5.,50gr Admire United States Pallasite Pallasite Slice 16.10gr Fragment 6.53gr Agen France Chondrite olivine bronzite H H5 Fragment 0.188gr Agost Espagne Limite K/T-clay layer Impactite Fragments 20.00gr Limite K/T-clay layer Fragments 20.00gr Agoult Maroc Achondrite Eucrite Eucrite Fragment 0.120gr Al Haggounia 001 Maroc Achondrite aubrite or Enstatite EL3 Individual 1.140gr Individual 1.002gr Individual 1.000gr Individual 710gr Fragments >600gr Al Mahbas Nord Ouest Afrique Pallasite Pallasite Individual 2.070gr Individual 1.38gr Alfianello Italia Chondrite oliv. Hypersthène L L6 Fragment 0.348gr Allan Hills 76009 ANTARCTIQUE Chondrite oliv. Hypersthène L L6 Fragments 0.56gr Allende Mexique Chondrite carbonée CV3 Slice 32.00gr Individual 5,25gr Almahabas NWA Achondrite lunar breccia Lunar Slice 0.740gr Anthraxolite Canada Impactite Impactite Individual 442gr Apt France Chondrite à olivine et hypersthène L6 Fragment 1.126gr Arizonite Tectite arizonite Tectite Individual 25.75gr Individual 21.20gr Individual 16.80gr Individual 12.85gr Atacama Chili Chondrite ? Fragment 162gr Aubres France Achondrite aubrite Aubrite Fragment 0.023gr Ausson France Chondrite à olivine et hypersthène L5 Fragment 0.258gr Australite Australia Tectite Tectite Rond 0.882gr Individual 1.640gr Individuals (100 pieces lot) 50.00gr Chips 5.00gr Australite BUTTON Australia Tectite Button ( moulage ) 2.07gr Azzuara Espagne Brèche d'impact Impactite Slice 278gr Babaudus France Brèche d'impact Impactite Endcut 27.00gr Barbotan France Chondrite olivine bronzite H5 Fragment 0.675gr Page 1 de 16 Bassikounou Chondrite H5 Fragment 11.870gr Bechar 001 Algérie Chondrite à olivine et hypersthène L7 Fragment 3.20gr Bediasites United States Tectite Tectite Individual 20.50gr Individual 16.50gr Individual 15.00gr Bendego Bresil Octaédrite IC Individual 14.00gr Bensour Algérie Chondrite transitoire L/LL LL6 Individual 12.50gr Berduc Argentina Chondrite à olivine et hytersthène L6 Individual 24.40gr Bicolite Philippines Tectite Tectite Individual 36.75gr Individual 33.55gr Individual 29.45gr Bilanga Burkina Faso Achondrite Diogénite Diogenite Fragment 1.200gr 0.300gr 0.210gr 0.250gr 0.245gr Bishopville United States Achondrite Aubrite Aubrite Fragment 0.200gr Bouvante France Achondrite Eucrite Eucrite Fragment 0.370gr Boxhole Australia Octaédrite moyenne IIIA Slice 12.70gr Brahin URSS Pallasite Pallasite Slice 83.00gr Brenham United States Pallasite Pallasite Slice 27.00gr Fragment 26.20gr Calcalong Creek Achondrite lunaire Lunar Fragment 0.001gr Fragment 0.001gr Camel Donga Australia Achondrite eucrite monomicte Eucrite-mmicte Individual 7.10gr Campo del Cielo Argentine Octaédrite grosse Iron, IAB-MG Slice 51.00gr Individual 4.176gr Canyon Diablo United States Octaédrite grosse IA Individual 530gr Individual 324gr Individual 212gr Individual 96.10gr Individual 63.25gr Oxyde 25.10gr Oxyde 23.00gr Oxyde 20.40gr Oxyde 19.00gr Individual 8.00gr Slice polished 14.50gr Cape York Greenland Octaédrite IIIAB Slice 13.20gr Carancas Pérou Chondrite H4-5 Fragment 0.610gr Page 2 de 16 Champagnac France Breche d'impact Impactite Slice 72.00gr Chantonnay France Chondrite à olivine et hypersthène L6 Fragment 0.633gr Charsonville France Chondrite H6 Fragment micro Chassenom France Brèche d'impact Impactite Fragment 204gr Brèches ~500gr Ramassage perso Fragments - slices lot > 2kg Chassigny France Achondrite Chassignite Martian chassignite Fragments 0.011gr Château-Renard France Chondrite à olivine et hytersthène L6 Fragment 0.608gr Chelyabinsk Russie Chondrite L5 L5 Individual 6.100gr Individual 4.250gr Individual 1.404gr Individual 1.256gr Individual 0.292gr Individual 0.252gr Individual 0.836gr Individual 0.272gr Individual 0.362gr Individual 0.360gr Individual 0.356gr Individual 0.345gr Individual 0.305gr Individual 0.272gr Chergach Mali Chondrite olivine bronzite H5 Individual Orient. 11.75gr Chiang Khan Thailande Chondrite olivine bronzite H6 Individual 8.,90gr Chinese tectite Chine Tectite Tectite Macro 115gr Box with 5 individual 19.60gr Chinga URSS Ataxite IVB-ANOM Slice 96.60gr Colombianite Colombie Tectite Tectite Individual 4.62gr Cumberland United States Achondrite aubrite Aubrite Fragment 0.264gr Dakhleh Glass Egypte Impactite Tectite Fragment 62.00gr Dalgety Down Australia Fragment 3.55gr Dar al Gani 056 Lybie Chondrite carbonée C3 Fragment 0.060gr Dar al Gani 225 Lybie Chondrite ord. H3.9 Slice 7.04gr Dar al Gani 262 Lybie LUNAR Lunar 2 fragments 0.028gr Dar al Gani 319 Lybie Achondrite Ureilite Ureilite Fragment 0.360gr Dar al Gani 400 Lybie Lunar Anorthosite bréciated Lunar Slice 0.144gr Slice 0.082gr Dar al Gani 476 Lybie Achondrite Shergottite Martian shergot. Slice 0.574gr Slice 0.046gr Page 3 de 16 Slice 0.004gr Dar al Gani 610 Lybie Chondrite ordinaire H H4 0.865gr Dar al Gani 670 Lybie Achondrite Shergottite Martian shergot. Slice 0.164gr Dar al Gani 671 Lybie Achondrite Howardite Howardite Slice 0.625gr Slice 0.685gr Dar al Gani 749 Lybie Chondrite carbonée CO3 Individual 3.00gr Darwin Glass Australia Tectite Tectite Fragment 5.00gr Fragment 6.94gr Lot de 5 fragments 14.55gr Dhofar 007 Oman Achondrite Eucrite Eucrite Crusted slice 15.10gr Dhofar 025 Oman Achondrite lunaire Lunar Fragment 0.003gr Dhofar 026 Oman Achondrite lunar anorth. cristalline breccia Lunar Fragment 0.005gr Slice 0.155gr Dhofar 081 Oman LUNAR ( Anorthositic Breccia LUN A ) Lunar Fragment 0.102gr Dhofar 700 Oman Achondrite Diogenite Diogénite Slice 5.45gr Dhofar 908 Oman Achondrite lunaire Lunar Fragment 0.050gr Dhofar 911 Oman Achondrite lunaire Lunar Fragment 0.020gr Fragment 0.024gr Dhofar1084 Oman Achondrite lunaire Lunar Fragment 0.010gr Dhofar1085 Oman Achondrite lunaire Lunar Slice 0.448gr Dhofar1303 Oman Achondrite ureilite Ureilite Slice 2.590gr Dimmit United States Chondrite olivine bronzite H H4 Individual 310gr Draveil France Chondrite olivine bronzite H H5 Fragments (2) micros El Hammani Mauritanie Chondrite olivine bronzite H H5 Slice 215gr Ensisheim France Amphotérite LL6 Slice 0.713gr Esnandes France Chondrite oliv. Hypersthène L L6 Fragments (2) 0.066gr Esquel Argentine Pallasite Pallasite Slice 14.00gr Slice 0.600gr Favars France Chondrite olivine bronzite H H5 Fragment micro Franconia United States Chondrite olivine bronzite H H4 Slice 13.750gr Individual 18.600gr Gaine County Park United States Chondrite oliv.bronzite H5 Slice 25.80gr Gao-Guenie Haute Volta Chondrite oliv.bronzite H6 Individual 155.00gr Slice 78.00gr Slice 44.00gr Individual 17.60gr Individual 10.50gr Individual 7.00gr Individual 10.40gr Individual 12.40gr Page 4 de 16 Individual 4.15gr Gebel Kamil Egypte Iron ungrouped Ataxite Individual 977.60gr 93.90gr Ghubara Oman Chondrite, Xénolithique L5 Individual 333.00gr Gibeon Namibie Octaédrite fine IVA Individual 1,480gr Slice 99.00gr Slice 26.00gr Slice 22.00gr Slice 21.00gr Slice 1.40gr Micro 2.00gr Micro 2.00gr Gibson Desert Australie Chondrite ? Individual 225.940gr Glorieta Mountain United States Pallasite Pallasite Individual 2.40gr Individual 3.80gr Glover Bluff Canada Brèche d'impact Impactite Tranche-talon 485.00gr Brèche (Red melt breccia) Impactite Slice 65.00gr Gold Bassin United States Chondrite oliv. Hypersthène L L4 Individual 264.00gr Governador Valadares Brésil Achondrite NAKLITE Martian Naklite Fragment 0.006gr Guang Dong Chine Tectite Tectite Individual 6.00gr Hainaut France Chondrite olivine bronzite H H3-H6 Slice 0.369gr Henbury Australia Octaédrite moyenne IIIA Individual 102gr Individual 38gr Individual 12.45gr 3 Minis 14.00gr Hoba Namibie Ataxite IVB Slice 1.70gr Fragment 0.640gr Slice 0.444gr Holbrook United States Chondrite oliv. Hypersthène L L6 Individual 7.00gr Fragment 1.42gr Individual 6.00gr Fragment 0.400gr Huckita Australia Pallasite Pallasite Individual 2.30gr Imilac Chini, Atacama Pallasite Pallasite Slice 6.576gr Individual 8.30gr Individual 4.70gr Individual 0.95gr Indochinite Tectite Tectite Rond 190.00gr Allongée 174.00gr Ovale 138.00gr Page 5 de 16 Ovale 118.00gr Ovale 77.00gr Forme de poire 62.00gr Lot divers 60.00gr Individual 5.00gr Individual 5.10gr Individual 13.00gr Individual 56.00gr Irghizite Tectite .00 50 pieces lot ~50.00gr Ivuna Tanzanie Chondrite carbonée CI Dust 0.050gr Jalu Lybie Chondrite veinée L6 Slice 22.50gr Jbilet Winselwan Maroc Chondrite carbonée CM2 Individual crusted 1.334gr Individual crusted 1.678gr Individual crusted 0.900gr Individual crusted 0.898gr Individual crusted 0.730gr Individual crusted 0.622gr Individual crusted 0.570gr Individual crusted 0.510gr Individual crusted 0.492gr Individual crusted 0.478gr Individual crusted 0.460gr Individual crusted 0.448gr Individual crusted 0.444gr Individual crusted 0.396gr Individual crusted 0.386gr Individual crusted 0.366gr Individual crusted 0.350gr Individual crusted 0.322gr Individual crusted 0.312gr Individual crusted 0.311gr Individual crusted 0.310gr Individual crusted 0.288gr Individual crusted 0.248gr Individual crusted 0.234gr Individual crusted 0.210gr Individual crusted 0.204gr Individual crusted 0.200gr Individual crusted 0.186gr Individual crusted 0.170gr Page 6 de 16 Individual crusted 0.170gr Individual crusted 0.168gr Individual crusted 0.130gr Individual crusted 0.104gr Individual crusted 0.100gr Individual crusted 0.096gr Individual
Recommended publications
  • Astronomy 150: Killer Skies Lecture 5, January 27

    Astronomy 150: Killer Skies Lecture 5, January 27

    Astronomy 150: Killer Skies Lecture 5, January 27 Last time: began Astro Threat I: Impacts Today: Meteors and Asteroids Homework: ‣ HW 1 due today, but allowing submission up until next Monday. ‣ HW 2 posted today, due next Friday at the start of class http://epod.usra.edu/blog/2011/01/fireball-breakup.html http://epod.usra.edu/blog/2011/05/willamette-meteorite.html Friday, January 27, 2012 Register your i>clicker Go to link on class web page to register your i>clicker ‣ Register with first part of your @illinois.edu email (NetID) If you can’t read your i>clicker ID ‣ Go the Illini bookstore bag-check counter ‣ Vote with your i>clicker ‣ Clicker ID will be displayed on the base unit https://online-s.physics.uiuc.edu/cgi/courses/shell/iclicker.pl Friday, January 27, 2012 Register your i>clicker Go to link on class web page to register your i>clicker ‣ Register with first part of your @illinois.edu email (NetID) If you can’t read your i>clicker ID ‣ Go the Illini bookstore bag-check counter ‣ Vote with your i>clicker ‣ Clicker ID will be displayed on the base unit https://online-s.physics.uiuc.edu/cgi/courses/shell/iclicker.pl Friday, January 27, 2012 Planetarium Session Purpose: ‣ To help you understand the motions of the sky Dates: 1/30, 1/31, 2/2, 2/6, 2/7, 2/8 @ Staerkel Planetarium, Parkland College ‣ Show starts at 7pm, runs ~80 minutes ‣ $3 door charge, please bring exact change Report due Feb 24th in class ‣ Details on class website ‣ Attach ticket from the show to your report Reserve a seat online ‣ Link to reservation site on class website Friday, January 27, 2012 Fireballs Since most meteors are from small objects, they burn up before they hit the ground.
  • Tubular Symplectic Inclusions in Olivine from the Fukang Pallasite

    Tubular Symplectic Inclusions in Olivine from the Fukang Pallasite

    Meteoritics & Planetary Science 45, Nr 5, 899–910 (2010) doi: 10.1111/j.1945-5100.2010.01054.x Tubular symplectic inclusions in olivine from the Fukang pallasite Michael R. STEVENS1, David R. BELL1,2, and Peter R. BUSECK1,2* 1School of Earth and Space Exploration, Arizona State University, Tempe, Arizona 85287, USA 2Department of Chemistry and Biochemistry, Arizona State University, Tempe, Arizona 85287, USA *Corresponding author. E-mail: [email protected] (Received 11 June 2009; revision accepted 27 March 2010) Abstract–Olivine from the Fukang meteorite, like that from many other pallasites, contains distinctive arrays of parallel, straight, tubular inclusions. They differ in their extension and linearity from those in terrestrial olivines. They comprise approximately 1% of the total volume. Most have lens-shaped cross-sections, but some are rounded. The major axis of the lens-shaped inclusions is rigorously oriented along olivine [001], and the rounded ones lie along olivine [010] and a few along [100]. The linear nature and orientations of the inclusions suggest that they nucleated on screw dislocations, perhaps formed through shock triggering. High-resolution transmission electron microscopy (TEM) and energy-dispersive x-ray spectroscopy show that the inclusions consist of symplectic intergrowths of chromite, diopside, and silica that appear to have formed by exsolution from the host olivine. The symplectites consist of chromite lamellae with approximately 35-nm spacings that grew outward from a central plane, with interstitial diopside and silica. Contrast modulations having an average spacing of 4.4 nm occur within the chromite lamellae. Using a reaction- front model, we estimate that exsolution occurred over a period of 30 to 100 min, suggesting rapid cooling at high temperature.
  • Nanomagnetic Properties of the Meteorite Cloudy Zone

    Nanomagnetic Properties of the Meteorite Cloudy Zone

    Nanomagnetic properties of the meteorite cloudy zone Joshua F. Einslea,b,1, Alexander S. Eggemanc, Ben H. Martineaub, Zineb Saghid, Sean M. Collinsb, Roberts Blukisa, Paul A. J. Bagote, Paul A. Midgleyb, and Richard J. Harrisona aDepartment of Earth Sciences, University of Cambridge, Cambridge, CB2 3EQ, United Kingdom; bDepartment of Materials Science and Metallurgy, University of Cambridge, Cambridge, CB3 0FS, United Kingdom; cSchool of Materials, University of Manchester, Manchester, M13 9PL, United Kingdom; dCommissariat a` l’Energie Atomique et aux Energies Alternatives, Laboratoire d’electronique´ des Technologies de l’Information, MINATEC Campus, Grenoble, F-38054, France; and eDepartment of Materials, University of Oxford, Oxford, OX1 3PH, United Kingdom Edited by Lisa Tauxe, University of California, San Diego, La Jolla, CA, and approved October 3, 2018 (received for review June 1, 2018) Meteorites contain a record of their thermal and magnetic history, field, it has been proposed that the cloudy zone preserves a written in the intergrowths of iron-rich and nickel-rich phases record of the field’s intensity and polarity (5, 6). The ability that formed during slow cooling. Of intense interest from a mag- to extract this paleomagnetic information only recently became netic perspective is the “cloudy zone,” a nanoscale intergrowth possible with the advent of high-resolution X-ray magnetic imag- containing tetrataenite—a naturally occurring hard ferromagnetic ing methods, which are capable of quantifying the magnetic state mineral that
  • (Sptpang Coil.) [I49] I50 Bulletin American Museum of Natural History

    (Sptpang Coil.) [I49] I50 Bulletin American Museum of Natural History

    Article VIII.-CATALOGUE OF METEORITES IN THE COLLECTION OF THE AMERICAN MUSEUM OF NATURAL HISTORY, TO JULY i, I896. By E. 0. HOVEY. 'T'he Collection of Meteorites in the Arnerican Museum of Natural History consists of fifty-five slabs, fragments and com- plete individuals, representing twenty-six falls and finds. The foundation of the mineralogical department of the Museum was laid in I874 by the purchase of the collection of S. C. H. Bailey, in which there were a few meteorites. More were acquired with the portion of the Norman Spang Collection of Minerals which was purchased in I89I, and other meteorites have been bought by the Museum from time to time, or have been presented to it by friends. The soujrce from which each specimen came has been indicated in the following cataloguLe. This publication is made to assist. the large number of persons who have become interested in knowing the extent to which the material of various falls and finds has been distributed among collections and the present location of specimens. AEROSIDERITES. (IRON METEORI ES.) Cat. Date of NAME AND Weight No. Discovery. DE;SCRIPTION. in grams. 18 1784 Tejupilco, Toluca Valley, Mexico. A complete individual, the surface of which has scaled off somewhat. A polished and etched surface shows coarse Widmanstatten figures. 1153. (Bailey Co/i.) 17841 Xiquipilco, Toluca Valley, Mexico. A complete individual of ellipsoidal form, which had been used as a pounder by the natives. 564. (Sptpang Coil.) [I49] I50 Bulletin American Museum of Natural History. [Vol. VIII, AEROSIDERITES.-Continued. Cat. Date of NAME AND DESCRIPTION.
  • Linking the Chassigny Meteorite and the Martian Surface Rock Backstay: Insights Into Igneous Crustal Differentiation Processes on Mars

    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.
  • Disequilibrium Melting and Melt Migration Driven by Impacts: Implications for Rapid Planetesimal Core Formation

    Disequilibrium Melting and Melt Migration Driven by Impacts: Implications for Rapid Planetesimal Core Formation

    Available online at www.sciencedirect.com Geochimica et Cosmochimica Acta 100 (2013) 41–59 www.elsevier.com/locate/gca Disequilibrium melting and melt migration driven by impacts: Implications for rapid planetesimal core formation Andrew G. Tomkins ⇑, Roberto F. Weinberg, Bruce F. Schaefer 1, Andrew Langendam School of Geosciences, P.O. Box 28E, Monash University, Melbourne, Victoria 3800, Australia Received 20 January 2012; accepted in revised form 24 September 2012; available online 12 October 2012 Abstract The e182W ages of magmatic iron meteorites are largely within error of the oldest solar system particles, apparently requir- ing a mechanism for segregation of metals to the cores of planetesimals within 1.5 million years of initial condensation. Cur- rently favoured models involve equilibrium melting and gravitational segregation in a static, quiescent environment, which requires very high early heat production in small bodies via decay of short-lived radionuclides. However, the rapid accretion needed to do this implies a violent early accretionary history, raising the question of whether attainment of equilibrium is a valid assumption. Since our use of the Hf–W isotopic system is predicated on achievement of chemical equilibrium during core formation, our understanding of the timing of this key early solar system process is dependent on our knowledge of the seg- regation mechanism. Here, we investigate impact-related textures and microstructures in chondritic meteorites, and show that impact-generated deformation promoted separation of liquid FeNi into enlarged sulfide-depleted accumulations, and that this happened under conditions of thermochemical disequilibrium. These observations imply that similar enlarged metal accumu- lations developed as the earliest planetesimals grew by rapid collisional accretion.
  • Metal-Silicate Fractionation and Chondrule Formation

    Metal-Silicate Fractionation and Chondrule Formation

    A756 Goldschmidt 2004, Copenhagen 6.3.12 6.3.13 Metal-silicate fractionation and Fe isotopes fractionation in chondrule formation: Fe isotope experimental chondrules 1 2 2,3 constraints S. LEVASSEUR , B. A. COHEN , B. ZANDA , 2 1 1 1 1 2 2 R.H. HEWINS AND A.N. HALLIDAY X.K. ZHU , Y. GUO , S.H. TANG , A. GALY , R.D. ASH 2 AND R.K O’NIONS 1 ETHZ, Dep. of Earth Sciences, Zürich, Switzerland ([email protected]) 1 Lab of Isotope Geology, MLR, Chinese Academy of 2 Rutgers University, Piscataway, NJ, USA Geological Sciences, 26Baiwanzhuang Road, Beijing, 3 Muséum National d’Histoire Naturelle, Paris, France China ([email protected]) 2 Department of Earth Sciences, Oxford University, Parks Road, Oxford, OX1 3PR, UK Natural chondrules show an Fe-isotopic mass fractionation range of a few δ-units [1,2] that is interpreted either as the result of Fe depletion from metal-silicate Recent studies have shown that considerable variations of fractionation during chondrule formation [1] or as the Fe isotopes exist in both meteoritic and terrestrial materials, reflection of the fractionation range of chondrule precursors and that they are related, through mass-dependent [2]. In order to better understand the iron isotopic fractionation, to a single isotopically homogeneous source[1]. compositions of chondrules we conducted experiments to This implies that the Fe isotope variations recorded in the study the effects of reduction and evaporation of iron on iron solar system materials must have resulted from mass isotope systematics. fractionation incurred by the processes within the solar system About 80mg of powdered slag fayalite was placed in a itself.

  • The History of the Hoba Meteorite III: Known and Loved by All

    the hoba meteorite The History of the Hoba Meteorite III: Known and loved by all ... P E Spargo Department of Physics, University of Cape Town, Rondebosch 7701, South Africa [email protected] In spite of its remote location in the However, apart from Luyten’s very brief then little-visited and almost unknown note in the Harvard College Observatory territory of South-West Africa (Namibia Bulletin (Luyten, 1929a, reproduced in today), we saw previously (Spargo facsimile in Fig. 8 in the second of this 2008b) that the second decade of the series of articles) and his short, largely great meteorite’s life opened with its descriptive articles in the South African existence being relatively widely known Journal of Science (Luyten 1929b) and to the public in South Africa and the Popular Astronomy (Luyten, 1930), noth- United States. This was as a result of ing of serious scientific import had been articles in Die Volksblad (Bloemfon- published. tein), The Cape Times (Cape Town), The Star (Johannesburg) and The New York It will be recalled, however, that on 5 Times1. There were also brief notes in September 1929 the meteorite had been Die Sterne (R.H., 1930), the popular visited by a small party of geologists who German astronomical magazine, which were on an excursion to Southwest Africa at least alerted German astronomers following the International Geological to its existence, and the Zeitschrift für Congress, which had held its XV Session Praktische Geologie (Schneiderhöhn, in South Africa in July and August of that 1929) performing a similar function for year.
  • Australian Aborigines and Meteorites

    Australian Aborigines and Meteorites

    Records of the Western Australian Museum 18: 93-101 (1996). Australian Aborigines and meteorites A.W.R. Bevan! and P. Bindon2 1Department of Earth and Planetary Sciences, 2 Department of Anthropology, Western Australian Museum, Francis Street, Perth, Western Australia 6000 Abstract - Numerous mythological references to meteoritic events by Aboriginal people in Australia contrast with the scant physical evidence of their interaction with meteoritic materials. Possible reasons for this are the unsuitability of some meteorites for tool making and the apparent inability of early Aborigines to work metallic materials. However, there is a strong possibility that Aborigines witnessed one or more of the several recent « 5000 yrs BP) meteorite impact events in Australia. Evidence for Aboriginal use of meteorites and the recognition of meteoritic events is critically evaluated. INTRODUCTION Australia, although for climatic and physiographic The ceremonial and practical significance of reasons they are rarely found in tropical Australia. Australian tektites (australites) in Aboriginal life is The history of the recovery of meteorites in extensively documented (Baker 1957 and Australia has been reviewed by Bevan (1992). references therein; Edwards 1966). However, Within the continent there are two significant areas despite abundant evidence throughout the world for the recovery of meteorites: the Nullarbor that many other ancient civilizations recognised, Region, and the area around the Menindee Lakes utilized and even revered meteorites (particularly of western New South Wales. These accumulations meteoritic iron) (e.g., see Buchwald 1975 and have resulted from prolonged aridity that has references therein), there is very little physical or allowed the preservation of meteorites for documentary evidence of Aboriginal acknowledge­ thousands of years after their fall, and the large ment or use of meteoritic materials.
  • (M = Ca, Mg, Fe2+), a Structural Base of Ca3mg3(PO4)4 Phosphors

    (M = Ca, Mg, Fe2+), a Structural Base of Ca3mg3(PO4)4 Phosphors

    crystals Article Crystal Chemistry of Stanfieldite, Ca7M2Mg9(PO4)12 (M = Ca, Mg, Fe2+), a Structural Base of Ca3Mg3(PO4)4 Phosphors Sergey N. Britvin 1,2,* , Maria G. Krzhizhanovskaya 1, Vladimir N. Bocharov 3 and Edita V. Obolonskaya 4 1 Department of Crystallography, Institute of Earth Sciences, St. Petersburg State University, Universitetskaya Nab. 7/9, 199034 St. Petersburg, Russia; [email protected] 2 Nanomaterials Research Center, Kola Science Center of Russian Academy of Sciences, Fersman Str. 14, 184209 Apatity, Russia 3 Centre for Geo-Environmental Research and Modelling, Saint-Petersburg State University, Ulyanovskaya ul. 1, 198504 St. Petersburg, Russia; [email protected] 4 The Mining Museum, Saint Petersburg Mining University, 2, 21st Line, 199106 St. Petersburg, Russia; [email protected] * Correspondence: [email protected] Received: 1 May 2020; Accepted: 25 May 2020; Published: 1 June 2020 Abstract: Stanfieldite, natural Ca-Mg-phosphate, is a typical constituent of phosphate-phosphide assemblages in pallasite and mesosiderite meteorites. The synthetic analogue of stanfieldite is used as a crystal matrix of luminophores and frequently encountered in phosphate bioceramics. However, the crystal structure of natural stanfieldite has never been reported in detail, and the data available so far relate to its synthetic counterpart. We herein provide the results of a study of stanfieldite from the Brahin meteorite (main group pallasite). The empirical formula of the mineral is Ca8.04Mg9.25Fe0.72Mn0.07P11.97O48. Its crystal structure has been solved and refined to R1 = 0.034. Stanfieldite from Brahin is monoclinic, C2/c, a 22.7973(4), b 9.9833(2), c 17.0522(3) Å, β 99.954(2)◦, 3 V 3822.5(1)Å .
  • Wednesday, March 22, 2017 [W453] MARTIAN METEORITE MADNESS: MIXING on a VARIETY of SCALES 1:30 P.M

    Wednesday, March 22, 2017 [W453] MARTIAN METEORITE MADNESS: MIXING on a VARIETY of SCALES 1:30 P.M

    Lunar and Planetary Science XLVIII (2017) sess453.pdf Wednesday, March 22, 2017 [W453] MARTIAN METEORITE MADNESS: MIXING ON A VARIETY OF SCALES 1:30 p.m. Waterway Ballroom 5 Chairs: Arya Udry Geoffrey Howarth 1:30 p.m. Nielsen S. G. * Magna T. Mezger K. The Vanadium Isotopic Composition of Mars and Evidence for Solar System Heterogeneity During Planetary Accretion [#1225] Vanadium isotope composition of Mars distinct from Earth and chondrites. 1:45 p.m. Tait K. T. * Day J. M. D. Highly Siderophile Element and Os-Sr Isotope Systematics of Shergotittes [#3025] The shergottite meteorites represent geochemically diverse, broadly basaltic, and magmatically-derived rocks from Mars. New samples were processed and analyzed. 2:00 p.m. Armytage R. M. G. * Debaille V. Brandon A. D. Agee C. B. The Neodymium and Hafnium Isotopic Composition of NWA 7034, and Constraints on the Enriched End-Member for Shergottites [#1065] Couple Sm-Nd and Lu-Hf isotopic systematics in NWA 7034 suggest that such a crust is not the enriched end-member for shergottites. 2:15 p.m. Howarth G. H. * Udry A. Nickel in Olivine and Constraining Mantle Reservoirs for Shergottite Meteorites [#1375] Ni enrichment in olivine from enriched versus depleted shergottites provide evidence for constraining mantle reservoirs on Mars. 2:30 p.m. Jean M. M. * Taylor L. A. Exploring Martian Mantle Heterogeneity: Multiple SNC Reservoirs Revealed [#1666] The objective of the present study is to assess how many mixing components can be recognized, and address ongoing debates within the martian isotope community. 2:45 p.m. Udry A. * Day J.
  • Lost Lake by Robert Verish

    Lost Lake by Robert Verish

    Meteorite-Times Magazine Contents by Editor Like Sign Up to see what your friends like. Featured Monthly Articles Accretion Desk by Martin Horejsi Jim’s Fragments by Jim Tobin Meteorite Market Trends by Michael Blood Bob’s Findings by Robert Verish IMCA Insights by The IMCA Team Micro Visions by John Kashuba Galactic Lore by Mike Gilmer Meteorite Calendar by Anne Black Meteorite of the Month by Michael Johnson Tektite of the Month by Editor Terms Of Use Materials contained in and linked to from this website do not necessarily reflect the views or opinions of The Meteorite Exchange, Inc., nor those of any person connected therewith. In no event shall The Meteorite Exchange, Inc. be responsible for, nor liable for, exposure to any such material in any form by any person or persons, whether written, graphic, audio or otherwise, presented on this or by any other website, web page or other cyber location linked to from this website. The Meteorite Exchange, Inc. does not endorse, edit nor hold any copyright interest in any material found on any website, web page or other cyber location linked to from this website. The Meteorite Exchange, Inc. shall not be held liable for any misinformation by any author, dealer and or seller. In no event will The Meteorite Exchange, Inc. be liable for any damages, including any loss of profits, lost savings, or any other commercial damage, including but not limited to special, consequential, or other damages arising out of this service. © Copyright 2002–2010 The Meteorite Exchange, Inc. All rights reserved. No reproduction of copyrighted material is allowed by any means without prior written permission of the copyright owner.