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Petrography and Mineral Chemistry of Escalón Meteorite, an H4 Chondrite, México
148 Reyes-SalasRevista Mexicana et al. de Ciencias Geológicas, v. 27, núm. 1, 2010, p. 148-161 Petrography and mineral chemistry of Escalón meteorite, an H4 chondrite, México Adela M. Reyes-Salas1,*, Gerardo Sánchez-Rubio1, Patricia Altuzar-Coello2, Fernando Ortega-Gutiérrez1, Daniel Flores-Gutiérrez3, Karina Cervantes-de la Cruz1, Eugenio Reyes4, and Carlos Linares5 1 Universidad Nacional Autónoma de México, Instituto de Geología, Del. Coyoacán, 04510 México D.F., Mexico. 2 Universidad Nacional Autónoma de México, Centro de Investigación en Energía, Campus Temixco, Priv. Xochicalco s/n, 62580 Temixco Morelos, Mexico. 3 Universidad Nacional Autónoma de México, Instituto de Astronomía, Del. Coyoacán, 04510 México D.F., Mexico. 4 Universidad Nacional Autónoma de México, Facultad de Química, Del. Coyoacán, 04510 México D.F., Mexico. 5 Universidad Nacional Autónoma de México, Instituto de Geofísica, Del. Coyoacán, 04510 México D.F., Mexico. * [email protected] ABSTRACT The Escalón meteorite, a crusted mass weighing 54.3 g, was recovered near Zona del Silencio in Escalón, state of Chihuahua, México. The stone is an ordinary chondrite belonging to the high iron group H, type 4. Electron microprobe analyses of olivine (Fa18.1) and pyroxene (Fs16.5), phosphate, plagioclase, opaque phases, matrix and chondrule glasses are presented. The metal phases present are kamacite (6.08 % Ni), taenite (31.66 % Ni), high nickel taenite (50.01 % Ni) and traces of native Cu. The chondrules average apparent diameter measures 0.62 mm. X-ray diffraction pattern shows olivine, pyroxene and kamacite. Alkaline-type glass is found mainly in chondrules. This meteorite is a stage S3, shock-blackened chondrite with weathering grade W0. -
NEW HIGH-PRECISION POTASSIUM ISOTOPES of TEKTITES. Y. Jiang1,2, H
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 1311.pdf NEW HIGH-PRECISION POTASSIUM ISOTOPES OF TEKTITES. Y. Jiang1,2, H. Chen2, B. Fegley, Jr.2, K. Lodders2, W. Hsu3, S. B. Jacobsen4, K. Wang (王昆)2. 1CAS Key Laboratory of Planetary Sciences, Purple Moun- tain Observatory, Chinese Academy of Sciences ([email protected]), 2Dept. Earth & Planetary Sciences and McDonnell Center for the Space Sciences, Washington University in St. Louis ([email protected]), 3Space Sci- ence Institute, Macau University of Science and Technology, 4Dept. Earth & Planetary Sciences, Harvard University. Introduction: Tektites are natural glassy objects crater of Hawaii (BHVO-1), are also analyzed. Hainan formed from the melting and rapid cooling of terrestri- Tektite is a typical splash-form tektite from Hainan al rocks during the high-energy impacts of meteorites, Island, China and of a dumbbell shape. We analyzed K comets, or asteroids upon the surface of the Earth [1]. isotopes of 15 chips along the longitudinal axis of its Chemical and isotopic compositions indicate that pre- profile, on a Neptune Plus MC-ICP-MS at Washington cursor components of tektites are the upper terrestrial University in St. Louis [14]. Except for Hainan tektite, continental crust, rather than extraterrestrial rocks. all other samples were only analyzed in bulk, with a Tektites are characterized by the depletion of volatile GV Instruments IsoProbe P MC-ICP-MS at Harvard elements and water, and heavy Cd, Sn, Zn and Cu iso- University following the description in [13]. K isotope topic compositions [2-5]. Since volatilities of elements compositions are reported using the per mil (‰) nota- 41 41 39 41 39 are defined by their 50% condensation temperature (Tc) tion, where δ K = ([( K/ K)sample/( K/ K)standard – of the solar nebula gas at 10-4 bars [6], there is no rea- 1]×1000). -
Zac Langdon-Pole
Zac Langdon-Pole Michael Lett 312 Karangahape Road Cnr K Rd & East St PO Box 68287 Newton Auckland 1145 New Zealand P+ 64 9 309 7848 [email protected] www.michaellett.com Zac Langdon-Pole Passport (Argonauta) (v) (front and side view) 2018 paper nautilus shell, Sericho meteorite (iron pallasite, landsite: Sericho, Kenya) 107 x 33 x 56mm ZL5210 Zac Langdon-Pole Residuals (c) 2018 Installation view, Between Bridges, Berlin February 2018 Zac Langdon-Pole Residuals (c) 2018 Installation view, Between Bridges, Berlin February 2018 Zac Langdon-Pole Ars Viva 2017/18 Installation view S.M.A.K., Ghent February 2018 Zac Langdon-Pole Ars Viva 2017/18 Installation view S.M.A.K., Ghent February 2018 Zac Langdon-Pole Ars Viva 2017/18 Installation view S.M.A.K., Ghent [offsite] February 2018 Zac Langdon-Pole Ars Viva 2017/18 Installation view S.M.A.K., Ghent February 2018 Zac Langdon-Pole Oratory Index Installation view Michael Lett, Auckland December 2016 Zac Langdon-Pole Oratory Index Installation view Michael Lett December 2016 Zac Langdon-Pole Installation view La Biennale de Montréal October 2016 Zac Langdon-Pole The Torture Garden 2016 framed digital print 620 x 490mm ZL4656 Zac Langdon-Pole 2017 Ars Viva 2018, Kunstverein München, Munich, Germany (group) Born 1988 Station, Melbourne, Australia (solo) Lives and works in Darmstadt and Berlin, Germany Vanished and Delft, Pah Homestead, Auckland, New Zealand (group) 2015 2016 Meisterschüler, Städelschule, Staatliche Hochschule für Bildende Künste. Prof. La Biennale de Montréal, Canada (group) -
A Review of Evidence for a Gulf of Tonkin Location for the Australasian Tektite Source Crater Aubrey Whymark* Consultant Wellsite Geologist, Manila, Philippines
Thai Geoscience Journal 2(2), 2021, p. 1-29 1 Copyright © 2021 by the Department of Mineral Resources of Thailand ISSN-2730-2695; DOI-10.14456/tgj.2021.2 A review of evidence for a Gulf of Tonkin location for the Australasian tektite source crater Aubrey Whymark* Consultant Wellsite Geologist, Manila, Philippines. *Corresponding author: [email protected] Received 5 March 2021; Accepted 17 June 2021. Abstract Australasian tektites (AAT) occur across Southeast Asia, Australia, the Indian Ocean, and southwest Pacific Ocean. AAT form the youngest and most extensive major tektite strewn field. Unlike other tektite strewn fields, AAT have no known source crater. Review of the literature establishes that a single ~ 43 km post-impact diameter crater exists, possibly significantly enlarged by slumping. The obliquity of the impact that formed the AAT would result in a crater that is less pervasive in depth but with greater downrange shock effects and melt ejection. Multiple lines of evidence, historically viewed in isolation, were examined, concatenated, contextualized, and discussed. Tektite morpho- logy and distribution; microtektite regressions; geochemical considerations, comparisons, and iso- -concentration regressions; lithological characteristics; age of source rock; and regional geological considerations are reviewed. The source material is predicted to be an abnormally thick sequence of rapidly deposited, poorly compacted, deltaic to shallow marine, shales to clay-rich siltstones of early Pleistocene to Pliocene age. The impact likely occurred in a shallow marine environment. Forty- two maps of positive and negative parameters are presented and overlain. These indicate the AAT source crater probably lies in the central to northwestern Yinggehai - Song Hong Basin / Gulf of Tonkin. -
Geological Survey Canada
70-66 GEOLOGICAL PAPER 70-66 ., SURVEY OF CANADA DEPARTMENT OF ENERGY, MINES AND RESOURCES REVISED CATALOGUE OF THE NATIONAL METEORITE COLLECTION OF CANADA LISTING ACQUISITIONS TO AUGUST 31, 1970 J. A. V. Douglas 1971 Price, 75 cents GEOLOGICAL SURVEY OF CANADA CANADA PAPER 70-66 REVISED CATALOGUE OF THE NATIONAL METEORITE COLLECTION OF CANADA LISTING ACQUISITIONS TO AUGUST 31, 1970 J. A. V. Douglas DEPARTMENT OF ENERGY, MINES AND RESOURCES @)Crown Copyrights reserved Available by mail from Information Canada, Ottawa from the Geological Survey of Canada 601 Booth St., Ottawa and Information Canada bookshops in HALIFAX - 1735 Barrington Street MONTREAL - 1182 St. Catherine Street West OTTAWA - 171 Slater Street TORONTO - 221 Yonge Street WINNIPEG - 499 Portage Avenue VANCOUVER - 657 Granville Street or through your bookseller Price: 75 cents Catalogue No. M44-70-66 Price subject to change without notice Information Canada Ottawa 1971 ABSTRACT A catalogue of the National Meteorite Collection of Canada, published in 1963 listed 242 different meteorite specimens. Since then specimens from 50 a dditional meteorites have been added to the collection and several more specimens have been added to the tektite collection. This report describes all specimens in the collection. REVISED CATALOGUE OF THE NATIONAL METEORITE COLLECTION OF CANADA LISTING ACQUISITIONS TO AUGUST 31, 1970 INTRODUCTION At the beginning of the nineteenth century meteorites were recog nized as unique objects worth preserving in collections. Increasingly they have become such valuable objects for investigation in many fields of scienti fic research that a strong international interest in their conservation and pre servation has developed (c. f. -
Noble Gas Study of the Saratov L4 Chondrite
Meteoritics & Planetary Science 45, Nr 3, 361–372 (2010) doi: 10.1111/j.1945-5100.2010.01026.x Noble gas study of the Saratov L4 chondrite Jun-ichi MATSUDA1*, Hidetomo TSUKAMOTO1, Chie MIYAKAWA1, and Sachiko AMARI2 1Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka 560-0043, Japan 2Laboratory for Space Sciences and the Physics Department, Washington University, St. Louis, Missouri 63130, USA *Corresponding author. E-mail: [email protected] (Received 10 September 2008; revision accepted 28 December 2009) Abstract–We have determined the elemental abundances and the isotopic compositions of noble gases in a bulk sample and an HF ⁄ HCl residue of the Saratov (L4) chondrite using stepwise heating. The Ar, Kr, and Xe concentrations in the HF ⁄ HCl residue are two orders of magnitude higher than those in the bulk sample, while He and Ne concentrations from both are comparable. The residue contains only a portion of the trapped heavy noble gases in Saratov; 40 ± 9% for 36Ar, 58 ± 12% for 84Kr, and 48 ± 10% for 132Xe, respectively. The heavy noble gas elemental pattern in the dissolved fraction is similar to that in the residue but has high release temperatures. Xenon isotopic ratios of the HF ⁄ HCl residue indicate that there is no Xe-HL in Saratov, but Ne isotopic ratios in the HF ⁄ HCl residue lie on a straight line connecting the cosmogenic component and a composition between Ne-Q and Ne-HL. This implies that the Ne isotopic composition of Q has been changed by incorporating Ne-HL (Huss et al. -
Asteroid Regolith Weathering: a Large-Scale Observational Investigation
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved. -
N Arieuican%Mllsellm
n ARieuican%Mllsellm PUBLISHED BY THE AMERICAN MUSEUM OF NATURAL HISTORY CENTRAL PARK WEST AT 79TH STREET, NEW YORK 24, N.Y. NUMBER 2I63 DECEMBER I9, I963 The Pallasites BY BRIAN MASON' INTRODUCTION The pallasites are a comparatively rare type of meteorite, but are remarkable in several respects. Historically, it was a pallasite for which an extraterrestrial origin was first postulated because of its unique compositional and structural features. The Krasnoyarsk pallasite was discovered in 1749 about 150 miles south of Krasnoyarsk, and seen by P. S. Pallas in 1772, who recognized these unique features and arranged for its removal to the Academy of Sciences in St. Petersburg. Chladni (1794) examined it and concluded it must have come from beyond the earth, at a time when the scientific community did not accept the reality of stones falling from the sky. Compositionally, the combination of olivine and nickel-iron in subequal amounts clearly distinguishes the pallasites from all other groups of meteorites, and the remarkable juxtaposition of a comparatively light silicate mineral and heavy metal poses a nice problem of origin. Several theories of the internal structure of the earth have postulated the presence of a pallasitic layer to account for the geophysical data. No apology is therefore required for an attempt to provide a comprehensive account of this remarkable group of meteorites. Some 40 pallasites are known, of which only two, Marjalahti and Zaisho, were seen to fall (table 1). Of these, some may be portions of a single meteorite. It has been suggested that the pallasite found in Indian mounds at Anderson, Ohio, may be fragments of the Brenham meteorite, I Chairman, Department of Mineralogy, the American Museum of Natural History. -
Meteorite Collections: Sample List
Meteorite Collections: Sample List Institute of Meteoritics Department of Earth and Planetary Sciences University of New Mexico October 01, 2021 Institute of Meteoritics Meteorite Collection The IOM meteorite collection includes samples from approximately 600 different meteorites, representative of most meteorite types. The last printed copy of the collection's Catalog was published in 1990. We will no longer publish a printed catalog, but instead have produced this web-based Online Catalog, which presents the current catalog in searchable and downloadable forms. The database will be updated periodically. The date on the front page of this version of the catalog is the date that it was downloaded from the worldwide web. The catalog website is: Although we have made every effort to avoid inaccuracies, the database may still contain errors. Please contact the collection's Curator, Dr. Rhian Jones, ([email protected]) if you have any questions or comments. Cover photos: Top left: Thin section photomicrograph of the martian shergottite, Zagami (crossed nicols). Brightly colored crystals are pyroxene; black material is maskelynite (a form of plagioclase feldspar that has been rendered amorphous by high shock pressures). Photo is 1.5 mm across. (Photo by R. Jones.) Top right: The Pasamonte, New Mexico, eucrite (basalt). This individual stone is covered with shiny black fusion crust that formed as the stone fell through the earth's atmosphere. Photo is 8 cm across. (Photo by K. Nicols.) Bottom left: The Dora, New Mexico, pallasite. Orange crystals of olivine are set in a matrix of iron, nickel metal. Photo is 10 cm across. (Photo by K. -
Population Polygons of Tektite Specific Gravity for Various Localities in Australasia
Reprinted from GEOCHIMICA ET COSMOCHIMICA ACTA Vol. 28, NO. 6,pp. 821-839 t II d 0 i (CA'TECORYI I {NASA CR OR TMX OR AD NUMBER1 ! POPULATION POLYGONS OF TEKTITE SPECIFIC GRAVITY FOR VARIOUS LOCALITIES IN AUSTRALASIA DEANR. CHAPMAN,HOWARD K. LARSONand LEROYC. SCHEIBER N.A.S.A., Ames Research Center, Moffett Field, California PERGAMON PRESS NEWYORK * OXFORD - LONDON - PARIS 1964 Geochimica et Cosmochimica Acta 1984, Val. 28, pp. 821 to 839. Pergamon Press Ltd. Printed in Northern Ireland Population polygons of tektite specific gravity for various localities in Australasia* DEANR. CHAPMAN,HOWARD K. LARSON and LEROYC. SCHEIBER N.A.S.A., Ames Research Ccnter, Moffett Field, California 31- Abstract-~Ieasurements of specific gravity by the method of liquid flotation have been made on about 6000 tektites from 18 different localities in Australasia, from 1 locality in Texas and 2 in Czechoslovakia. Comparison of specific-gravity population polygons for various localities has led to the unanticipated conclusion that the amtralite population in southwest Australia is essentially the same as the philippinite population, rather than the population elsewhere in Australia. The javanite population appears closely related to certain populations in Australia. In several localities the presence of two superimposed populations is demonstrated. The specific- gravity evidence indicates that the Australasian tektites represent a single event comprising many distinguishable clusters, some of which have partially overlapped. INTRODUCTION #e AT the turn of this century, the Austrian geologist SUESS(1900) gave the collective name of “tektites” to three widely separated groups of natural glass objects then known to be scattered over parts of Australia, Czechoslovakia and the island of Billiton. -
Chondrules and Their Origins. Subject Index
359 1983chto.conf..359. SUBJECT INDEX Ablation spherules 21 formation 46, 50 as chondrule analogs 11, 22 internal isochrons 251, 256 composition 14, 15, 17, 18 iodine-xenon dating 256 formation 11-14, 19 matrix ages 257 grains 13, 14 metamorphic structure 47 iron 14 origin 50 magnetic properties 15 photomicrographs 47 matrix 13 potassium-argon dating 251 melting 19, 21, 22 texture 44 metals 19 ultrathin sections 47 mineralogy 19 Allende chondrules photomicrographs 13 ages 247-251,253,255-257 porphyritic 21 alteration 159 siderophiles 15-19 cavities 155-157, 159 texture 19 classification 207 thermal effects 12-14 composition 42, 93, 156, 157 volatiles 13, 14 EPMA 93 Aerodynamic spherules extraction temperature 254 as chondrule analogs 10, 12 formation 160 composition 12 iodine 254, 256, 257 formation 12 iodine-xenon 258 thermal effects 12 isochrons 254 Age dating techniques 257 isotopes 37, 39-42, 270 iodine-xenon 246, 247 mineralogy 93, 149-152, 154, 155, 158, 160 isochrons 257 mixing line 41 metamorphic processes 257 opaque inclusions 155, 159 potassium-argon 246, 247 photomicrographs 148, 150, 151, 154, 156, rubidium-strontium 246, 247 157 uranium-lead 246, 247 precursors 42 Ages of chondrules sample analysis 39 iodine-xenon 246, 247, 251-257 SEM studies 150, 151, 152, 154, 156, 157 potassium-argon 246, 247, 250, 251, 257, 258 texture 39, 41, 155 rubidium-strontium 246-250, 258 thermal history 255 uranium-lead 246-248, 258 xenon closure 254 Allegan Allende inclusions 145 bulk analysis of chondrules 48, 49 ages 255 chemistry 46 initial iodine 256· chondrule ages 251, 256, 257 iodine-xenon dating 255 chondrule oxygen isotope analysis 40 isochrons 255 chondrules 44, 47 isotope analysis 39 classification 46, 50 sample analysis 39 composition 46 texture 39 description 46 Allende matrix 145, 257 equilibration 44, 50 alteration 159 © Lunar and Planetary Institute • Provided by the NASA Astrophysics Data System 360 Chondrules and their Origins 1983chto.conf..359. -
Isotopic Fractionation of Zn in Tektites
Isotopic fractionation of Zn in tektites Frederic Moynier1, 2,*, Pierre Beck3, Fred Jourdan4, Qing-zhu Yin2, Christian Koeberl5, and Uwe Reimold6 1Department of Earth and Planetary Sciences, Washington University in St Louis, One Brookings Drive, St Louis, MO 63130 2Department of Geology, University of California Davis. One Shields Avenue, Davis, CA 95616 3Laboratoire de Planetologie, Universite Joseph Fourier, CNRS/INSU, Bat. Physique D, BP 53, 38041 Grenoble cedex 9, France 4 Western Australian Argon Isotope Facility, Department of Applied Geology & JdL-CMS, Curtin university of Technology, GPO Box U1987, Perth, WA 6845; Australia. 5Department of Lithospheric Research, University of Vienna, Althanstrasse 14, A-1090 Vienna, Austria 6Museum f. Natural History (Mineralogy), Humbold University Berlin, Invalidenstrasse 43, 10115 Berlin, Germany *Corresponding author: [email protected], Tel: +1 314-935-8634, Fax: +1 314-935-7361 Abstract: Tektites are terrestrial natural glasses, produced during a hypervelocity impact of an asteroid (or comet nucleus) into the Earth surface. The similarity between the chemical and isotopic compositions of tektites and terrestrial upper continental crust implies they formed from the target rocks. The mechanism of the loss of water as well as the behavior of volatile species during tektites formation is still debated, and volatilization at high temperature is a possible way. Volatilization can fractionate isotopes, and, therefore, comparing the isotope composition of volatile elements in tektites with their source rocks may help to understand the conditions of evaporation. In this study, we have measured the Zn isotopic composition of 20 tektites from the four different strewn fields. Almost all the samples are enriched in heavy isotopes of Zn compared to the upper continental crust.