Bartoschewitz - Catalogue of Meteorites
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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. -
Meteorites, Asteroids, and Comets
Space Sci Rev (2018) 214:36 https://doi.org/10.1007/s11214-018-0474-9 Water Reservoirs in Small Planetary Bodies: Meteorites, Asteroids, and Comets Conel M.O’D. Alexander1 · Kevin D. McKeegan2 · Kathrin Altwegg3 Received: 10 January 2018 / Accepted: 11 January 2018 / Published online: 23 January 2018 © Springer Science+Business Media B.V., part of Springer Nature 2018 Abstract Asteroids and comets are the remnants of the swarm of planetesimals from which the planets ultimately formed, and they retain records of processes that operated prior to and during planet formation. They are also likely the sources of most of the water and other volatiles accreted by Earth. In this review, we discuss the nature and probable origins of asteroids and comets based on data from remote observations, in situ measurements by spacecraft, and laboratory analyses of meteorites derived from asteroids. The asteroidal par- ent bodies of meteorites formed ≤ 4 Ma after Solar System formation while there was still a gas disk present. It seems increasingly likely that the parent bodies of meteorites spectro- scopically linked with the E-, S-, M- and V-type asteroids formed sunward of Jupiter’s orbit, while those associated with C- and, possibly, D-type asteroids formed further out, beyond Jupiter but probably not beyond Saturn’s orbit. Comets formed further from the Sun than any of the meteorite parent bodies, and retain much higher abundances of interstellar mate- rial. CI and CM group meteorites are probably related to the most common C-type asteroids, and based on isotopic evidence they, rather than comets, are the most likely sources of the H and N accreted by the terrestrial planets. -
Recent Observations of the Soils on the Moon
Lunar Soil for a Myriad of Purposes and Products: Science, Engineering, and Applications LawrenceLawrence A.A. TaylorTaylor PPlanetary Geosciences Institute University of Tennessee Objectives NEW LUNAR SAMPLES UNIQUE PROPERTIES OF LUNAR SOIL NEW LUNAR MINERALS UNIQUE ABILITIES OF MICROWAVE RADIATION MICROWAVE PROCESSING OF LUNAR SOIL PRODUCTS FOR “THE BUSH LUNAR BASE” Newly Recovered Planetary Materials Meteorites from Antarctica Japan and USA Meteorites from Hot Deserts French Entrepreneurs in the Sahara Russian Entrepreneurs in Oman Meteorites as samples of : as well as Mars & Asteroidal Matter SEARCHING FOR METEORITES IN THE OMAN DESERT When viewed with binoculars, the Black Spot in the sand is: a) a ‘coke can’ [alcohol is verboten!]; b) evidence that a camel has stopped there recently; or c) a dark-colored rock [fusion crust on a meteorite]. Meteorite? LunarLunar MeteoritesMeteorites fromfrom OmanOman Dhofar 287 Dhofar 025 (Impact-Melt Breccia) (Basalt + Breccia) Regolith Breccia Dhofar 301 Dhofar 302 Dhofar 303 New Lunar Rocks and Minerals: Farside Samples of the Moon South Pole / Amundsen Site Volcanic Glass Impact-Glass Lunar Mare Soil Bead Bead Agglutinate Rock Chips Impact Glass 1 mm Plagioclase Our Unhappy Moon MicrometeoriteMicrometeorite ImpactsImpacts onon LunarLunar GlassGlass BeadBead 5 µm Impact Craters LunarLunar SoilSoil FormationFormation Comminution, Agglutination, & Vapor Deposition TheThe onlyonly WeatheringWeathering andand EErosionalrosional agentagent onon thethe MoonMoon isis MeteoriteMeteorite andand MicrometeoriteMicrometeorite -
Moon Minerals a Visual Guide
Moon Minerals a visual guide A.G. Tindle and M. Anand Preliminaries Section 1 Preface Virtual microscope work at the Open University began in 1993 meteorites, Martian meteorites and most recently over 500 virtual and has culminated in the on-line collection of over 1000 microscopes of Apollo samples. samples available via the virtual microscope website (here). Early days were spent using LEGO robots to automate a rotating microscope stage thanks to the efforts of our colleague Peter Whalley (now deceased). This automation speeded up image capture and allowed us to take the thousands of photographs needed to make sizeable (Earth-based) virtual microscope collections. Virtual microscope methods are ideal for bringing rare and often unique samples to a wide audience so we were not surprised when 10 years ago we were approached by the UK Science and Technology Facilities Council who asked us to prepare a virtual collection of the 12 Moon rocks they loaned out to schools and universities. This would turn out to be one of many collections built using extra-terrestrial material. The major part of our extra-terrestrial work is web-based and we The authors - Mahesh Anand (left) and Andy Tindle (middle) with colleague have build collections of Europlanet meteorites, UK and Irish Peter Whalley (right). Thank you Peter for your pioneering contribution to the Virtual Microscope project. We could not have produced this book without your earlier efforts. 2 Moon Minerals is our latest output. We see it as a companion volume to Moon Rocks. Members of staff -
I-Xe Analysis of Enstatite Meteorites and a Eucrite
Testing an integrated chronology: I-Xe analysis of enstatite meteorites and a eucrite Item Type Article; text Authors Busfield, A.; Turner, G.; Gilmour, J. D. Citation Busfield, A., Turner, G., & Gilmour, J. D. (2008). Testing an integrated chronology: IXe analysis of enstatite meteorites and a eucrite. Meteoritics & Planetary Science, 43(5), 883-897. DOI 10.1111/j.1945-5100.2008.tb01087.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 26/09/2021 21:32:45 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656429 Meteoritics & Planetary Science 43, Nr 5, 883–897 (2008) AUTHOR’S PROOF Abstract available online at http://meteoritics.org Testing an integrated chronology: I-Xe analysis of enstatite meteorites and a eucrite A. BUSFIELD, G. TURNER, and J. D. GILMOUR* School of Earth, Atmospheric and Environmental Science, University of Manchester, Oxford Road, Manchester M13 9PL, UK *Corresponding author. E-mail: [email protected] (Supplementary tables and figures are available online at http://meteoritics.org/online supplements.htm) (Received 06 October 2006; revision accepted 21 November 2007) Abstract–We have determined initial 129I/127I ratios for mineral concentrates of four enstatite meteorites and a eucrite. In the case of the enstatite meteorites the inferred ages are associated with the pyroxene-rich separates giving pyroxene closure ages relative to the Shallowater standard of Indarch (EH4, 0.04 ± 0.67 Ma), Khairpur (EL6, −4.22 ± 0.67 Ma), Khor Temiki (aubrite, −0.06 Ma), and Itqiy (enstatite achondrite, −2.6 ± 2.6 Ma), negative ages indicate closure after Shallowater. -
18Th EANA Conference European Astrobiology Network Association
18th EANA Conference European Astrobiology Network Association Abstract book 24-28 September 2018 Freie Universität Berlin, Germany Sponsors: Detectability of biosignatures in martian sedimentary systems A. H. Stevens1, A. McDonald2, and C. S. Cockell1 (1) UK Centre for Astrobiology, University of Edinburgh, UK ([email protected]) (2) Bioimaging Facility, School of Engineering, University of Edinburgh, UK Presentation: Tuesday 12:45-13:00 Session: Traces of life, biosignatures, life detection Abstract: Some of the most promising potential sampling sites for astrobiology are the numerous sedimentary areas on Mars such as those explored by MSL. As sedimentary systems have a high relative likelihood to have been habitable in the past and are known on Earth to preserve biosignatures well, the remains of martian sedimentary systems are an attractive target for exploration, for example by sample return caching rovers [1]. To learn how best to look for evidence of life in these environments, we must carefully understand their context. While recent measurements have raised the upper limit for organic carbon measured in martian sediments [2], our exploration to date shows no evidence for a terrestrial-like biosphere on Mars. We used an analogue of a martian mudstone (Y-Mars[3]) to investigate how best to look for biosignatures in martian sedimentary environments. The mudstone was inoculated with a relevant microbial community and cultured over several months under martian conditions to select for the most Mars-relevant microbes. We sequenced the microbial community over a number of transfers to try and understand what types microbes might be expected to exist in these environments and assess whether they might leave behind any specific biosignatures. -
Aluminium-Mg Systematics of Winonaites and Differentiation of the Iab-Winonaite Parent Body
77th Annual Meteoritical Society Meeting (2014) 5155.pdf ALUMINIUM-MG SYSTEMATICS OF WINONAITES AND DIFFERENTIATION OF THE IAB-WINONAITE PARENT BODY. Y. Hidaka1, V. Debaille1 and G. Hublet1. 1Laboratoire G-Time, Université Libre de Bruxelles, Brussels, Belgium. Introduction: Primitive achondrites such as winonaites are important materials to investigate the early differentiation processes of asteroids. Winonaites are considered to originate from the same parent body than IAB non-magmatic iron meteorites [1]. Short-lived radionuclide chronometers are useful to understand the first few million years of the solar system history. The Al-Mg system is one of the most established short- lived systematics that provides a very good time resolution. Previous Hf-W isotopic studies have revealed that IAB- winonaite parent body had accreted ~1 Ma after CAI formation [2] and its magmatic activity ceased ~4 Ma later [3]. However, there is no other chronological data of winonaites from other short-lived radionuclide systems, in particular from fully lithophile systematics, as W is siderophile. Therefore, we consider here additional Al-Mg chronological data of winonaites to investigate the early evolutionary history of the silicate portion of their parent body. Results and Discussion: We have investigated two winonaite meteorites NWA 725 and Y-8005, with a present focus on the first one. NWA 725 is officially classified as an acapulcoite, but oxygen isotopic data of this meteorite indicated that NWA 725 and paired meteorites are actually winonaites [4, 5]. NWA 725 has been reported as chondrule-bearing, the least metamorphosed primitive achondrite [6]. The evolutionary models of IAB-winonaite parent body [1, 2] indicated that this parent body should preserve intact, chondritic areas during partial melting and silicate-metal segregation processes. -
Iron Isotope Cosmochemistry Kun Wang Washington University in St
Washington University in St. Louis Washington University Open Scholarship All Theses and Dissertations (ETDs) 12-2-2013 Iron Isotope Cosmochemistry Kun Wang Washington University in St. Louis Follow this and additional works at: https://openscholarship.wustl.edu/etd Part of the Earth Sciences Commons Recommended Citation Wang, Kun, "Iron Isotope Cosmochemistry" (2013). All Theses and Dissertations (ETDs). 1189. https://openscholarship.wustl.edu/etd/1189 This Dissertation is brought to you for free and open access by Washington University Open Scholarship. It has been accepted for inclusion in All Theses and Dissertations (ETDs) by an authorized administrator of Washington University Open Scholarship. For more information, please contact [email protected]. WASHINGTON UNIVERSITY IN ST. LOUIS Department of Earth and Planetary Sciences Dissertation Examination Committee: Frédéric Moynier, Chair Thomas J. Bernatowicz Robert E. Criss Bruce Fegley, Jr. Christine Floss Bradley L. Jolliff Iron Isotope Cosmochemistry by Kun Wang A dissertation presented to the Graduate School of Arts and Sciences of Washington University in partial fulfillment of the requirements for the degree of Doctor of Philosophy December 2013 St. Louis, Missouri Copyright © 2013, Kun Wang All rights reserved. Table of Contents LIST OF FIGURES ....................................................................................................................... vi LIST OF TABLES ........................................................................................................................ -
Faculty Publications and Creative Works 2003 Office of Theice V President for Research
University of New Mexico UNM Digital Repository Office of the Vice President for Research Archives & University Administrative Records 2003 Faculty Publications and Creative Works 2003 Office of theice V President for Research Follow this and additional works at: https://digitalrepository.unm.edu/ovp_research_publications Recommended Citation Office of the Vice President for Research. "Faculty Publications and Creative Works 2003." (2003). https://digitalrepository.unm.edu/ ovp_research_publications/21 This Report is brought to you for free and open access by the Archives & University Administrative Records at UNM Digital Repository. It has been accepted for inclusion in Office of the Vice President for Research by an authorized administrator of UNM Digital Repository. For more information, please contact [email protected]. ANDERSON SCHOOLS OF MANAGEMENT: SCHOOL OF PUBLIC ADMINISTRATION Rivera, Mario A. “Planeación e Integración Estratégica: Un Modelo con Estudio de Caso del Sector Judicial,” Estado, Gobierno, Gestión Pública 2 (4) 2003-2004, published June 2003. Coauthor Bruce Perlman. Applied Strategic Performance Management, P4 Management Solutions, 2003. Coauthor: Ted Vecchio. 197 pages. Varma, Roli Guest Editor, “Special Issue on Women and Minorities in Information Technology,” IEEE Technology and Society Magazine, 22(3). “E. F. Schumacher: Changing the Paradigm of Bigger Is Better.” Bulletin of Science, Technology and Society, 23(2), pp. 114-124. “Asians in the U.S. Public Service: Diversity, Achievements, and Glass Ceiling,” in Sumathi Reddy (ed.) Workforce Diversity: Concepts and Cases, pp. 26-42. Hyderabad: ICFAI University Press. 13 SCHOOL OF ARCHITECTURE AND PLANNING Adams, Geoffrey C. Exhibition: The HOME House Project, Southeast Center for Contemporary Art, Winston-Salem, North Carolina. May 10-July 6, 2003, David J. -
'San Juan', a New Mass of the Campo Del Cielo Meteorite Shower
‘San Juan’, a new mass of the Campo del Cielo meteorite shower Marcela Eliana SAAVEDRA1, María Eugenia VARELA1, Andrew J. CAMPBELL 2 and Dan TOPA 3 1Instituto de Ciencias Astronómicas de la Tierra y del Espacio (ICATE)-CONICET, San Juan, Argentina. 2Deptartment of the Geophysical Sciences, University of Chicago, , Chicago, USA. 3Central Research Laboratories, Natural History Museum, , Vienna, Austria. Email: [email protected] Editor: Diego A. Kietzmann Recibido: 19 de marzo de 2021 Aceptado: 15 de junio de 2021 Disponible online: 15 de junio de 2021 ABSTRACT Petrographic and chemical (major, minor and trace element) studies of silicate inclusions and metal from the San Juan A and B samples revealed that they are new masses belonging to the Campo del Cielo IAB iron meteorite shower. These masses must have being transported from the large strewn field in the Chaco and Santiago del Estero Provinces to the surroundings of San Juan city, where they have being recover in the year 2000. The sizes of the two masses of San Juan, collected 770 km SW from Santiago del Estero, is in agreement with the previously suggested anthropic hypothesis for the transport of Campo del Cielo. Keywords: IAB iron meteorites, Campo del Cielo meteorite, San Juan meteorite. RESUMEN San Juan, una nueva masa de la lluvia de meteoritos de Campo del Cielo Estudios petrográficos y químicos (elementos mayores, menores y trazas) de inclusiones de silicatos y de metal de las muestras A y B de San Juan, reveló que son nuevas masas que pertenecen a la lluvia de meteoritos de Campo del Cielo. -
A New Primitive Achondrite from Northwest Africa
A New Primitive Achondrite from Northwest Africa Kseniya K. Androsova* University of Calgary, Calgary, AB, Canada [email protected] and Alan R. Hildebrand University of Calgary, Calgary, AB, Canada Summary The winonaite and acapulcoite/lodranite meteorites constitute small groups of primitive achondrites that have experienced thermal metamorphism sometimes accompanied by varying degrees of partial melting. Petrographic and elemental abundance studies [optical microscope observations and electron microprobe analysis] have been conducted on several meteorites recovered in Northwest Africa (NWA). One meteorite has fine-grained, granulitic texture, abundant, evenly distributed metal and troilite grains, and highly reduced mineral compositions [Olivine (Fa6.0±0.4), low-Ca pyroxene (Fs7.5±0.4, Wo1.3±0.2), high-Ca pyroxene (Fs3.2±0.2, Wo45.8±0.7)]. Based on these criteria it appears that the data are consistent with the sample being a winonaite. The overall textural resemblance of this meteorite to NWA 1463 and /or NWA 725 (somewhat anomalous) winonaites (both having multiple relict chondrules) may suggest that this meteorite is paired with one or both. Although, until its oxygen isotope composition is obtained the classification of this meteorite as a winonaite (vs. as an acapulcoite) remains uncertain, its primitive achondritic nature is quite evident. Introduction The winonaite meteorites represent a class of rare primitive achondrites (together with the acapulcoite/lodranite association) that have sometimes undergone partial melting but generally have chondritic mineralogy and composition. Winonaites can be characterized by fine- to medium-grained, mostly granulitic textures, highly reduced mineral compositions, and unique oxygen isotope signatures (Benedix et al., 1998). Although most of the winonaites lack chondrules, several have been reported to have regions containing relict chondrules. -
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.