Subject Index.Fm

Total Page:16

File Type:pdf, Size:1020Kb

Subject Index.Fm Meteoritics & Planetary Science 38, Nr 12, 1877–1878 (2003) http://meteoritics.org Annual Subject Index 26Al-26Mg relative ages 939 CM chondrites 813 Frictional melting 1521 26Mg excess 5 Coalescence 49 Geochemistry, brachinites 1601 40Ar-39Ar dating 555, 887 Cometary meteorites 1045 Geochemistry, Mars 1849 Ablation 1023 Comets 457, 1283 Grain 49 Accretion 1399 Cosmic dust flux 1351 Grain boundary 1669, 1679 Accretionary rims 813 Continuous flow isotope ratio mass Graphite 767 Acfer 182 spectrometer 1255 Hebe, asteroid 711 Achondrite(s) 95, 145, 157 Copernicus secondary craters 13 HH064 145 Achondrites, brachinites 1601 Complex impact structure 445 Hibonite 5 Achondrites, differentiated 1485 Core formation 1425 Hughes 030 5 Achondrites, primitive 1485 Cosmic-ray exposure ages 1243, 1485 Hydrated minerals 1383 Aenigmatite 725 Cosmic-ray exposure history 157 Hydrogen 357 Ages, 39Ar-40Ar 341, 1601 Cosmic spherules 329 Hydrothermal alteration 365 Airwave 989 Composition of meteorites 1005 Ice flow 1319 Albite 725 Cosmogenic nuclides 157 IDPs 1585 Allan Hills icefield 1319 Cratering 905 IDPs/chondrites 1283 ALH 84001 109, 849, 1697 Crater clusters 905 IIIAB Alkaline-rich clasts Crater fill deposits 1437 IIIAB iron meteorites 117 26Al 35 Creep 427 Impact 747 Amino acids 399 Cretaceous-tertiary boundary 1299 Impact basins 565 Amorphous carbon 767 Crust 895 Impact breccia 1079 Annealing 1499, 1507 Crustal magnetization 565 Impact crater(s) 1137, 1299, 1341, 1551 Antarctic meteorite(s) 109, 831 Cumulate(s) 529, 1753 Impact cratering 13, 1255, 1641 Apollo 15 515 Dark inclusion 1399 Impact ejecta 1137 Asteroid(s) 383, 427, 1243, 1533 Dark streaks 1181 Impact glasses 1641 Asteroid composition 1053 Dating 1697 Impact heating 1499 Atmospheric entry heating 1627 Density 1161, 1533 Impact-induced 1521 Australasian tektite strewn field 1351 Dhofar 287 485 Impact-melt breccia 1507 Basalt generation 1807 Diamond 767 Impact melting 1507 Basin ejecta modeling 13 Dicarboxylic acids 357 Impact microcraters 1351 Bishunpur meteorites 59 Dust 457 Impact tectonics 1093 Botsumtwi crater, Ghana 1137 Dynamic crystallization 1263 Impact vaporization 383 Bolides 905 EH chondrites 389 INAA 783 Brachinites 1601 Electron microscopy 831 Infrasound 989 Brecciation 1499 Elements, major and trace 1713 Ion probe 1697 Bulk chemical compositions 939 Eros, asteroid 1053 IR spectra 49 CAIs 5, 35, 407 Exchange rate 357 Iron meteroites 1425 Calcalong Creek 595 Experimental petrology 95, 515, 1713 Isotope geochemistry 1713 Carbonaceous chondrite(s) 357, 407 Experimental trace element partitioning 1425 Isotopes; neodymium, strontium, oxygen 1793 Carbonate 831, 849 Exposure age 759 Isotopic composition-neodymium Carbonate melts 1299, 1641 Eucrite(s) 783 Isotopic composition-strontium 1079 Cataclysm, evidence against 579 Fabric rotatation 1093 Jalanash 145 Cathodoluminescence 1187 Falls 975, 1023 Jurassic (early) 445 Central European strewn field 887 Fassaite 407 Kamacite nucleation 1669 Central uplift 1093, 1341 Fe local structure 1181 KREEP 485, 529 CH chondrites 1199 Fe oxidation state 1181 Laboratory 457 Chemical zoning 1217 Ferric iron 1733 Laboratory model 1331 Chiral 357 Ferromagnesian chondrules 939 Libyan Desert glass 1181 Chicxulub 1079 Fine-grained rims 59 Lightning discharge 399 Chondrite(s) 341, 739, 1243 Fireball(s) 975, 989 LIL elements 895 Chondrites, LL 59 Fission Xe 627 Liquid immiscibility 1641 Chondrule formation 81 Fissure 1451 Lithological interface 1451 Chondrules 35, 59, 813 Flourine contamination 759 Lonar crater 365 Chondrules origin 927 Fluid dynamics 1331 Low probe 35 Chronology 341 Forsterite 49 Low temperature 399 Clay minerals 1437 Fractional condensation 1199 Lunar basin ejecta 13 Clementine 1461 Fragmentation 905, 1023 Lunar differentiation 515 1877 © Meteoritical Society, 2003. Printed in USA. 1878 Annual Subject Index, Volume 38, 2003 Lunar gardening 1351 Neon enrichment 747 Rotation 1331 Lunar mare basalts 501 Ningqiang carbonaceous chondrite 35 Rumuruti chondrite 5, 341 Lunar meteorite(s) 485, 501, 529, 595 Nitrogen 627 Sampling 1045 Lunar petrogenesis 515 Noble gas(es) 747, 767, 1005, 1243, 1485, 1627 Satellite aperture radar interferometry 1319 Lunar petrology 501 Noble gases, radiogenic 157 Secondary chondrules 927 Lunar Prospector spacecraft 565 Novaya Zemlya 329 Seismic 989 Lunar samples 595 Nuclear microprobe 1585 Shergottite(s) 725, 1815, 1833, 1849, 1865 Lunar terranes 595 Nuclear reaction 759 Shock 739, 1187 Lunar volcanism 555 Numerical simulation 1451 Shock barometry 1187 Macrodeformation 1109 NWA 032 555 Shock effects 1499, 1507 Magma ocean 1753, 1807 NWA 428 1499 Shock heating 1451 Magma production 1815 NWA 773 555 Shock loading 1451 Magnetic fields 565 Oblique impact 1551 Shock metamorphism 1109, 1137, 1341, 1579, Magnetite 831, 849 Olivine 81, 427, 813, 871, 1217 1865 Mantle, Mars 1793, 1849 Optical constants 419 Shock-produced diamond 1255 Mantle convection 1815 Orbits 975, 1005 Shocked quartz 1187, 1341 Mantle differentiation 1753 Ordinary chondrite, L4 157 Siderophile elements 1425 Mantle metasomatism 1849 Ordinary chondrite(s) 711, 795, 939, 963, 975, Silica 1199 Mare basalt 485, 529, 1461 1161, 1521, 1533, 1679 Silicates 457 Mare meteorites 555 Organic matter 795 Silicate melt 1263 Marine impact 1437 Orthopyroxene 871 SIMS 117 Mars 365, 831, 849, 871, 895, 905, 1697, 1713, Oxygen fugacity 1733, 1793 Smelting 95 1733, 1753, 1793, 1807, 1815, 1833 Oxygen isotopes 389 SNC meteorites 109, 895, 1733, 1793, 1807 Martensite 1669 PGE 1109 Solar wind 627, 1627 Martian (SNC) meteorites 871, 1865 Paleofield intensity 399 Space weathering 383, 1053 Matrix 1399 Pallasite(s) 427, 1217 Spade meteorite 1507 Megaregolith, evolution model 579 Parameterization of partition coeffiecients 1425 Spectral reflectance 1053 Melting 407 Partial melting 95 Spectroscopy 1283 Melt condensates 1263 Partitioning 1263 Splash-form 1331 Melt pocket 739, 1865 Petrogenetic model 1713 Stishovite 1579 Melt veins 1521 Petrology, brachinites 1601 Stony meteorites 1161 Melt, volcanic 1833 Phaeton 1045 Strewn field 1023 Metal(s) 59, 389, 1669 Phosphates 117, 1217 Suevite 1137, 1299 Metal formation 81 Picritic glasses 515 Super paramagnetic 399 Metal particles 1679 Planar deformation features 445 Surface enrichment 759 Meteors 1283 Planetary evolution 1753 Tagish Lake meteorite 419, 1585 Meteor shower (Geminids) 1045 Polycyclic aromatic hydrocarbons 109 Tektite(s) 747, 887, 1331, 1351 Meteorite(s) 963, 1533 Porosity 927, 1161, 1533 TEM 81, 157, 1199 Meteorite fall 989 Post-impact alteration 1109 Thermal decomposition 849 Meteorite classification 783 Post-impact deposits 1437 Thermal emission spectroscopy 871 Meteorite concentration sites 1319 Pressure effects on carbon isotope Thermal metamophism 795 Meteorite ejecta 1351 fractionation 1255 Thermal modeling 711 Meteorite impacts 1351 Primitive achondrites 783 TOF-SIMS 109 Meteorite shower 157 Primitive mantle 895 Trace element 595 Meteoroids 1005, 1045, 1283 Primordial noble gases 1399 Ureilite(s) 95, 145, 157, 767 Microimpacts 1351 Pseudotachylite 1521 Ureilite diamonds 1255 Micrometeorites 329, 1585, 1627 Pseudotachylitic breccia 1093 Venus 1551 Micro-Raman 1199 Pyroclastic rock 927 Vesta 427 Microtektites 1351 Pyroxene 389 Volatiles 383 Mineralogy 1243 QUE 94201 1833 Volcanism 1461, 1833 Mineralogy, asteroids 1383 Quench crystallization 1641 Vredefort impact structure 1093 Mn-Cr chronology 117 R-chondrite 341 Water content 1383 Model porosity 1161 Radiogenic heat production 1807 Weathering 759 Molten planetesimals 927 Raman spectroscopy 795, 1187 Whitlockite 1697 Moon 383, 529, 565, 1351,1461, 1551 Rare earth elements 783 Wilkinsonite 725 Moon, megaregolith evolution 579 REE microdistribution 1217 Woodleigh impact structure 1109 Moon, regolith evolution 579 Reduction 81 Wyoming 445 Morávka meteorite 989 Reflectance spectra 1383 Xanes 1181 Morávka 975, 1005, 1023 Refractive indices 419 Xenon 627 Mössbauer spectroscopy 963, 1733 Refractory forsterite 1263 X-ray diffraction 1627 Muong Nong-type 747 Refractory inclusions 813 Yanzhuang 739 Muonionalusta meteorite 1579 Regolith breccia 501 Yucàtan 1079 Murchison 1585 Regolith processes 627 Zoneless plessite 1679 NEAR spacecraft 1053 Remote sensing 1461 Nebula 407 Rims 1399.
Recommended publications
  • Constraints on the Water, Chlorine, and Fluorine Content of the Martian Mantle
    Meteoritics & Planetary Science 1–13 (2016) doi: 10.1111/maps.12624 Constraints on the water, chlorine, and fluorine content of the Martian mantle 1* 2,3 4 Justin FILIBERTO , Juliane GROSS , and Francis M. MCCubbin 1Department of Geology, Southern Illinois University, 1259 Lincoln Dr, MC 4324, Carbondale, Illinois 62901, USA 2Department of Earth and Planetary Sciences, Rutgers University, 610 Taylor Road, Piscataway, New Jersey 08854, USA 3Department of Earth and Planetary Sciences, The American Museum of Natural History, New York, New York 10024, USA 4NASA Johnson Space Center, Mail Code XI2, 2101 NASA Parkway, Houston, Texas 77058, USA *Corresponding author. E-mail: fi[email protected] (Received 30 July 2015; revision accepted 22 January 2016) Abstract–Previous estimates of the volatile contents of Martian basalts, and hence their source regions, ranged from nearly volatile-free through estimates similar to those found in terrestrial subduction zones. Here, we use the bulk chemistry of Martian meteorites, along with Martian apatite and amphibole chemistry, to constrain the volatile contents of the Martian interior. Our estimates show that the volatile content of the source region for the Martian meteorites is similar to the terrestrial Mid-Ocean-Ridge Mantle source. Chlorine is enriched compared with the depleted terrestrial mantle but is similar to the terrestrial enriched source region; fluorine is similar to the terrestrial primitive mantle; and water is consistent with the terrestrial mantle. Our results show that Martian magmas were not volatile saturated; had water/chlorine and water/fluorine ratios ~0.4–18; and are most similar, in terms of volatiles, to terrestrial MORBs. Presumably, there are variations in volatile content in the Martian interior as suggested by apatite compositions, but more bulk chemical data, especially for fluorine and water, are required to investigate these variations.
    [Show full text]
  • Magnetite Biomineralization and Ancient Life on Mars Richard B Frankel* and Peter R Buseckt
    Magnetite biomineralization and ancient life on Mars Richard B Frankel* and Peter R Buseckt Certain chemical and mineral features of the Martian meteorite with a mass distribution unlike terrestrial PAHs or those from ALH84001 were reported in 1996 to be probable evidence of other meteorites; thirdly, bacterium-shaped objects (BSOs) ancient life on Mars. In spite of new observations and up to several hundred nanometers long that resemble fos­ interpretations, the question of ancient life on Mars remains silized terrestrial microorganisms; and lastly, 10-100 nm unresolved. Putative biogenic, nanometer magnetite has now magnetite (Fe304), pyrrhotite (Fel_xS), and greigite (Fe3S4) become a leading focus in the debate. crystals. These minerals were cited as evidence because of their similarity to biogenic magnetic minerals in terrestrial Addresses magnetotactic bacteria. *Department of Physics, California Polytechnic State University, San Luis Obispo, California 93407, USA; e-mail: [email protected] The ancient life on Mars hypothesis has been extensively tDepartments of Geology and Chemistry/Biochemistry, Arizona State challenged, and alternative non-biological processes have University, Tempe, Arizona 85287-1404, USA; e-mail: [email protected] been proposed for each of the four features cited by McKay et al. [4]. In this paper we review the current situa­ tion regarding their proposed evidence, focusing on the Abbreviations putative biogenic magnetite crystals. BCM biologically controlled mineralization BIM biologically induced mineralization BSO bacterium-shaped object Evidence for and against ancient Martian life PAH polycyclic aromatic hydrocarbon PAHs and BSOs Reports of contamination by terrestrial organic materials [5°,6°] and the similarity of ALH84001 PAHs to non-bio­ genic PAHs in carbonaceous chondrites [7,8] make it Introduction difficult to positively identify PAHs of non-terrestrial, bio­ A 2 kg carbonaceous stony meteorite, designated genic origin.
    [Show full text]
  • 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.
    [Show full text]
  • March 21–25, 2016
    FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk,
    [Show full text]
  • Organic Matter in Meteorites Department of Inorganic Chemistry, University of Barcelona, Spain
    REVIEW ARTICLE INTERNATIONAL MICROBIOLOGY (2004) 7:239-248 www.im.microbios.org Jordi Llorca Organic matter in meteorites Department of Inorganic Chemistry, University of Barcelona, Spain Summary. Some primitive meteorites are carbon-rich objects containing a vari- ety of organic molecules that constitute a valuable record of organic chemical evo- lution in the universe prior to the appearance of microorganisms. Families of com- pounds include hydrocarbons, alcohols, aldehydes, ketones, carboxylic acids, amino acids, amines, amides, heterocycles, phosphonic acids, sulfonic acids, sugar-relat- ed compounds and poorly defined high-molecular weight macromolecules. A vari- ety of environments are required in order to explain this organic inventory, includ- ing interstellar processes, gas-grain reactions operating in the solar nebula, and hydrothermal alteration of parent bodies. Most likely, substantial amounts of such Received 15 September 2004 organic materials were delivered to the Earth via a late accretion, thereby provid- Accepted 15 October 2004 ing organic compounds important for the emergence of life itself, or that served as a feedstock for further chemical evolution. This review discusses the organic con- Address for correspondence: Departament de Química Inorgànica tent of primitive meteorites and their relevance to the build up of biomolecules. Universitat de Barcelona [Int Microbiol 2004; 7(4):239-248] Martí i Franquès, 1-11 08028 Barcelona, Spain Tel. +34-934021235. Fax +34-934907725 Key words: primitive meteorites · prebiotic chemistry · chemical evolution · E-mail: [email protected] origin of life providing new opportunities for scientific advancement. One Introduction of the most important findings regarding such bodies is that comets and certain types of meteorites contain organic mole- Like a carpentry shop littered with wood shavings after the cules formed in space that may have had a relevant role in the work is done, debris left over from the formation of the Sun origin of the first microorganisms on Earth.
    [Show full text]
  • A Magnetic Susceptibility Database for Stony Meteorites
    Direttore Enzo Boschi Comitato di Redazione Cesidio Bianchi Tecnologia Geofisica Rodolfo Console Sismologia Giorgiana De Franceschi Relazioni Sole-Terra Leonardo Sagnotti Geomagnetismo Giancarlo Scalera Geodinamica Ufficio Editoriale Francesca Di Stefano Istituto Nazionale di Geofisica e Vulcanologia Via di Vigna Murata, 605 00143 Roma Tel. (06) 51860468 Telefax: (06) 51860507 e-mail: [email protected] A MAGNETIC SUSCEPTIBILITY DATABASE FOR STONY METEORITES Pierre Rochette1, Leonardo Sagnotti1, Guy Consolmagno2, Luigi Folco3, Adriana Maras4, Flora Panzarino4, Lauri Pesonen5, Romano Serra6 and Mauri Terho5 1Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy [[email protected]] 2Specola Vaticana, Castel Gandolfo, Italy 3Antarctic [PNRA] Museum of Siena, Siena, Italy 4Università La Sapienza, Roma, Italy 5University of Helsinki, Finland 6“Giorgio Abetti” Museum of San Giovanni in Persiceto, Italy Pierre Rochette et alii: A Magnetic Susceptibility Database for Stony Meteorites 1. Introduction the Museo Nationale dell’Antartide in Siena [Folco and Rastelli, 2000], the University of More than 22,000 different meteorites Roma “la Sapienza” [Cavaretta Maras, 1975], have been catalogued in collections around the the “Giorgio Abetti” Museum in San Giovanni world (as of 1999) of which 95% are stony types Persiceto [Levi-Donati, 1996] and the private [Grady, 2000]. About a thousand new meteorites collection of Matteo Chinelatto. In particular, are added every year, primarily from Antarctic the Antarctic Museum in Siena is the curatorial and hot-desert areas. Thus there is a need for centre for the Antarctic meteorite collection rapid systematic and non-destructive means to (mostly from Frontier Mountain) recovered by characterise this unique sampling of the solar the Italian Programma Nazionale di Ricerche in system materials.
    [Show full text]
  • CHAPTER 1 Introduction
    Chemical analysis of organic molecules in carbonaceous meteorites Torrao Pinto Martins, Zita Carla Citation Torrao Pinto Martins, Z. C. (2007, January 24). Chemical analysis of organic molecules in carbonaceous meteorites. Retrieved from https://hdl.handle.net/1887/9450 Version: Corrected Publisher’s Version Licence agreement concerning inclusion of doctoral License: thesis in the Institutional Repository of the University of Leiden Downloaded from: https://hdl.handle.net/1887/9450 Note: To cite this publication please use the final published version (if applicable). ______________________________________________________ CHAPTER 1 ______________________________________________________ Introduction 1.1 Heavenly stones-from myth to science Ancient chronicles, from the Egyptian, Chinese, Greek, Roman and Sumerian civilizations documented the fall1 of meteorites, with Sumerian texts from around the end of the third millennium B. C. describing possibly one of the earliest words for meteoritic iron (Fig. 1.1 Left). Egyptian hieroglyphs meaning “heavenly iron” (Fig. 1.1 Right) found in pyramids together with the use of meteoritic iron in jewellery and artefacts show the importance of meteorites in early Egypt. Meteorites were worshiped by ancient Greeks and Romans, who struck coins to celebrate their fall, with the cult to worship meteorites prevailing for many centuries. For example, some American Indian tribes paid tribute to large iron meteorites, and even in modern days the Black Stone of the Ka´bah in Mecca is worshiped and regarded by Muslims as “an object from heaven”. The oldest preserved meteorite that was observed to fall (19th May 861) was found recently (October 1979) in a Shinto temple in Nogata, Japan. It weighted 472 g and it was stored in a wooden box.
    [Show full text]
  • Meteoroids: the Smallest Solar System Bodies
    Passage of Bolides through the Atmosphere 1 O. Popova Abstract Different fragmentation models are applied to a number of events, including the entry of TC3 2008 asteroid in order to reproduce existing observational data. keywords meteoroid entry · fragmentation · modeling 1 Introduction Fragmentation is a very important phenomenon which occurs during the meteoroid entry into the atmosphere and adds more drastic effects than mere deceleration and ablation. Modeling of bolide 6 fragmentation (100 – 10 kg in mass) may be divided into several approaches. Detail fitting of observational data (deceleration and/or light curves) allows the determination of some meteoroid parameters (ablation and shape-density coefficients, fragmentation points, amount of mass loss) (Ceplecha et al. 1993; Ceplecha and ReVelle 2005). Observational data with high accuracy are needed for the gross-fragmentation model (Ceplecha et al. 1993), which is used for the analysis of European and Desert bolide networks data. Hydrodynamical models, which describe the entry of the meteoroid 6 including evolution of its material, are applied mainly for large bodies (>10 kg) (Boslough et al. 1994; Svetsov et al. 1995; Shuvalov and Artemieva 2002, and others). Numerous papers were devoted to the application of standard equations for large meteoroid entry in the attempts to reproduce dynamics and/or radiation for different bolides and to predict meteorite falls. These modeling efforts are often supplemented by different fragmentation models (Baldwin and Sheaffer, 1971; Borovi6ka et al. 1998; Artemieva and Shuvalov, 2001; Bland and Artemieva, 2006, and others). The fragmentation may occur in different ways. For example, few large fragments are formed. These pieces initially interact through their shock waves and then continue their flight independently.
    [Show full text]
  • Processing of Meteoritic Organic Materials As a Possible Analog of Early Molecular Evolution in Planetary Environments
    Processing of meteoritic organic materials as a possible analog of early molecular evolution in planetary environments Sandra Pizzarelloa,1, Stephen K. Davidowskia, Gregory P. Hollanda, and Lynda B. Williamsb aDepartment of Chemistry and Biochemistry, Arizona State University, Tempe, AZ 85287-1604; and bSchool of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404 Edited* by Jonathan I. Lunine, Cornell University, Ithaca, NY, and approved August 2, 2013 (received for review May 14, 2013) The composition of the Sutter’s Mill meteorite insoluble organic hydrocarbons; several of these have identical counterparts in the material was studied both in toto by solid-state NMR spectroscopy terrestrial biosphere and have been extensively studied and of the powders and by gas chromatography–mass spectrometry reviewed (2). The IOM represents the larger portion of CC or- analyses of compounds released upon their hydrothermal treat- ganic carbon, up to 99%, and is not known in molecular detail. It ment. Results were compared with those obtained for other mete- is often referred to as kerogen-like because, like kerogen, it is orites of diverse classifications (Murray, GRA 95229, Murchison, insoluble and isolated after dissolution of free compounds and Orgueil, and Tagish Lake) and found to be so far unique in regard minerals by repeated washes with strong acids (4). The IOM bulk to the molecular species released. These include, in addition to O- composition can be only inferred from spectroscopy, e.g., NMR containing aromatic compounds, complex polyether- and ester- and infrared, or decomposition studies, which have suggested containing alkyl molecules of prebiotic appeal and never detected a complex macromolecular structure with both aromatic and in meteorites before.
    [Show full text]
  • 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.
    [Show full text]
  • Team Studies Rare Meteorite Possibly from the Outer Asteroid Belt 20 December 2012
    Team studies rare meteorite possibly from the outer asteroid belt 20 December 2012 The asteroid approached on an orbit that still points to the source region of CM chondrites. From photographs and video of the fireball, Jenniskens calculated that the asteroid approached on an unusual low-inclined almost comet-like orbit that reached the orbit of Mercury, passing closer to the sun than known from other recorded meteorite falls. "It circled the sun three times during a single orbit of Jupiter, in resonance with that planet," Jenniskens said. Based on the unusually short time that the asteroid was exposed to cosmic rays, there was not much time to go slower or faster around the sun. That puts the original source asteroid very (Phys.org)—Scientists found treasure when they close to this resonance, in a low inclined orbit. studied a meteorite that was recovered April 22, 2012 at Sutter's Mill, the gold discovery site that "A good candidate source region for CM chondrites led to the 1849 California Gold Rush. Detection of now is the Eulalia asteroid family, recently the falling meteorites by Doppler weather radar proposed as a source of primitive C-class asteroids allowed for rapid recovery so that scientists could in orbits that pass Earth," adds Jenniskens. study for the first time a primitive meteorite with little exposure to the elements, providing the most pristine look yet at the surface of primitive asteroids. An international team of 70 researchers reported in today's issue of Science that this meteorite was classified as a Carbonaceous-Mighei or CM-type carbonaceous chondrite and that they were able to identify for the first time the source region of these meteorites.
    [Show full text]
  • The Amino Acid Composition of the Sutterв•Žs Mill CM2 Carbonaceous
    University of Nebraska - Lincoln DigitalCommons@University of Nebraska - Lincoln NASA Publications National Aeronautics and Space Administration 2014 The minoa acid composition of the Sutter’s Mill CM2 carbonaceous chondrite Aaron Burton 1NASA Johnson Space Center, [email protected] Daniel Glavin NASA Goddard Space Flight Center Jamie Elsila NASA Goddard Space Flight Center Jason Dworkin NASA Goddard Space Flight Center Peter Jenniskens SETI Institute, NASA Ames Research Center See next page for additional authors Follow this and additional works at: http://digitalcommons.unl.edu/nasapub Burton, Aaron; Glavin, Daniel; Elsila, Jamie; Dworkin, Jason; Jenniskens, Peter; and Yin, Qing-Zhu, "The minoa acid composition of the Sutter’s Mill CM2 carbonaceous chondrite" (2014). NASA Publications. 134. http://digitalcommons.unl.edu/nasapub/134 This Article is brought to you for free and open access by the National Aeronautics and Space Administration at DigitalCommons@University of Nebraska - Lincoln. It has been accepted for inclusion in NASA Publications by an authorized administrator of DigitalCommons@University of Nebraska - Lincoln. Authors Aaron Burton, Daniel Glavin, Jamie Elsila, Jason Dworkin, Peter Jenniskens, and Qing-Zhu Yin This article is available at DigitalCommons@University of Nebraska - Lincoln: http://digitalcommons.unl.edu/nasapub/134 Meteoritics & Planetary Science 1–13 (2014) doi: 10.1111/maps.12281 The amino acid composition of the Sutter’s Mill CM2 carbonaceous chondrite Aaron S. BURTON1* , Daniel P. GLAVIN2, Jamie E. ELSILA2, Jason P. DWORKIN2, Peter JENNISKENS3,4, and Qing-Zhu YIN5 1NASA Johnson Space Center, 2101 Space Center Parkway, Houston, Texas 77058, USA 2NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, Maryland 20771, USA 3SETI Institute, 189 Bernardo Avenue, Mountain View, California 94043, USA 4NASA Ames Research Center, Moffett Field, California 94035, USA 5Department of Earth and Planetary Sciences, University of California at Davis, Davis, California 95616, USA *Corresponding author.
    [Show full text]