A Meteorite Perspective on Asteroid Hazard Mitigation
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The Villalbeto De La Peña Meteorite Fall: II. Determination of Atmospheric Trajectory and Orbit
Meteoritics & Planetary Science 41, Nr 4, 505–517 (2006) Abstract available online at http://meteoritics.org The Villalbeto de la Peña meteorite fall: II. Determination of atmospheric trajectory and orbit Josep M. TRIGO-RODRÍGUEZ1, 2*, JiÚí BOROVIª.$3, Pavel SPURNÝ3, José L. ORTIZ4, José A. DOCOBO5, Alberto J. CASTRO-TIRADO4, and Jordi LLORCA2, 6 1Institut de Ciències de l’Espai (ICE-CSIC), Campus UAB, Facultat de Ciències, Torre C-5, parells, 2a planta, 08193 Bellaterra (Barcelona), Spain 2Institut d’Estudis Espacials de Catalunya (IEEC), Ed. Nexus, Gran Capità 2-4, 08034 Barcelona, Spain 3Astronomical Institute of the Academy of Sciences, OndÚHMRY2EVHUYDWRU\&]HFK5HSXEOLF 4Instituto de Astrofísica de Andalucía (IAA-CSIC), P.O. Box 3004, 18080 Granada, Spain 5Observatorio Astronómico Ramón Maria Aller, Universidade de Santiago de Compostela, Spain 6Institut de Tècniques Energètiques, Universitat Politècnica de Catalunya, Diagonal 647, 08028 Barcelona, Spain *Corresponding author. E-mail: [email protected] (Received 23 April 2005; revision accepted 3 November 2005) Abstract–The L6 ordinary chondrite Villalbeto de la Peña fall occurred on January 4, 2004, at 16:46: 45 r 2 s UTC. The related daylight fireball was witnessed by thousands of people from Spain, Portugal, and southern France, and was also photographed and videotaped from different locations of León and Palencia provinces in Spain. From accurate astrometric calibrations of these records, we have determined the atmospheric trajectory of the meteoroid. The initial fireball velocity, calculated from measurements of 86 video frames, was 16.9 r 0.4 km/s. The slope of the trajectory was 29.0 r 0.6° to the horizontal, the recorded velocity during the main fragmentation at a height of 27.9 r 0.4 km was 14.2 r 0.2 km/s, and the fireball terminal height was 22.2 r 0.2 km. -
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. -
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, -
Did a Comet Deliver the Chelyabinsk Meteorite?
EPSC Abstracts Vol. 11, EPSC2017-2, 2017 European Planetary Science Congress 2017 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2017 Did a Comet Deliver the Chelyabinsk Meteorite? O.G. Gladysheva Ioffe Physical-Technical Institute of RAS, St.Petersburg, Russa, ([email protected] / Fax: +7(812)2971017) Abstract source of the appearance of such a gradient can be only the direct bombardment of the crystal by SCR An explosion of a celestial body occurred on the iron nuclei with energy of 1-100 MeV [6]. fifteenth of February, 2013, near Chelyabinsk Interacting with the surface of the meteorite, protons (Russia). The explosive energy was determined as and helium GCR nuclei form isotopes, some ~500 kt of TNT, on the basis of which the mass of radioactive, which are allocated to a specific location the bolide was estimated at ~107 kg, and its diameter by depth in the body of the meteorite. A measurement of the composition of radionuclides at ~19 m [1]. Fragments of the meteorite, such as 22 26 54 60 LL5/S4-WO type ordinary chondrite [2] with a total Na, Al, Mn and Co in 12 fragments of the mass only of ~2·103 kg, fell to the earth’s surface [3]. Chelyabinsk meteorite, and a comparison of the Here, we will demonstrate that the deficit of the results with model calculations of the formation of celestial body’s mass can be explained by the arrival these isotopes in meteorites according to depth, of the Chelyabinsk chondrite on Earth by a showed that 4 fragments of the meteorite were significantly more massive but fragile ice-bearing located in a layer 30 cm deep, 3 fragments at a depth celestial body. -
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. -
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. -
Radar-Enabled Recovery of the Sutter's Mill Meteorite, A
RESEARCH ARTICLES the area (2). One meteorite fell at Sutter’sMill (SM), the gold discovery site that initiated the California Gold Rush. Two months after the fall, Radar-Enabled Recovery of the Sutter’s SM find numbers were assigned to the 77 me- teorites listed in table S3 (3), with a total mass of 943 g. The biggest meteorite is 205 g. Mill Meteorite, a Carbonaceous This is a tiny fraction of the pre-atmospheric mass, based on the kinetic energy derived from Chondrite Regolith Breccia infrasound records. Eyewitnesses reported hearing aloudboomfollowedbyadeeprumble.Infra- Peter Jenniskens,1,2* Marc D. Fries,3 Qing-Zhu Yin,4 Michael Zolensky,5 Alexander N. Krot,6 sound signals (table S2A) at stations I57US and 2 2 7 8 8,9 Scott A. Sandford, Derek Sears, Robert Beauford, Denton S. Ebel, Jon M. Friedrich, I56US of the International Monitoring System 6 4 4 10 Kazuhide Nagashima, Josh Wimpenny, Akane Yamakawa, Kunihiko Nishiizumi, (4), located ~770 and ~1080 km from the source, 11 12 10 13 Yasunori Hamajima, Marc W. Caffee, Kees C. Welten, Matthias Laubenstein, are consistent with stratospherically ducted ar- 14,15 14 14,15 16 Andrew M. Davis, Steven B. Simon, Philipp R. Heck, Edward D. Young, rivals (5). The combined average periods of all 17 18 18 19 20 Issaku E. Kohl, Mark H. Thiemens, Morgan H. Nunn, Takashi Mikouchi, Kenji Hagiya, phase-aligned stacked waveforms at each station 21 22 22 22 23 Kazumasa Ohsumi, Thomas A. Cahill, Jonathan A. Lawton, David Barnes, Andrew Steele, of 7.6 s correspond to a mean source energy of 24 4 24 2 25 Pierre Rochette, Kenneth L. -
Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery and Characterization
O. P. Popova, et al., Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery and Characterization. Science 342 (2013). Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery, and Characterization Olga P. Popova1, Peter Jenniskens2,3,*, Vacheslav Emel'yanenko4, Anna Kartashova4, Eugeny Biryukov5, Sergey Khaibrakhmanov6, Valery Shuvalov1, Yurij Rybnov1, Alexandr Dudorov6, Victor I. Grokhovsky7, Dmitry D. Badyukov8, Qing-Zhu Yin9, Peter S. Gural2, Jim Albers2, Mikael Granvik10, Läslo G. Evers11,12, Jacob Kuiper11, Vladimir Kharlamov1, Andrey Solovyov13, Yuri S. Rusakov14, Stanislav Korotkiy15, Ilya Serdyuk16, Alexander V. Korochantsev8, Michail Yu. Larionov7, Dmitry Glazachev1, Alexander E. Mayer6, Galen Gisler17, Sergei V. Gladkovsky18, Josh Wimpenny9, Matthew E. Sanborn9, Akane Yamakawa9, Kenneth L. Verosub9, Douglas J. Rowland19, Sarah Roeske9, Nicholas W. Botto9, Jon M. Friedrich20,21, Michael E. Zolensky22, Loan Le23,22, Daniel Ross23,22, Karen Ziegler24, Tomoki Nakamura25, Insu Ahn25, Jong Ik Lee26, Qin Zhou27, 28, Xian-Hua Li28, Qiu-Li Li28, Yu Liu28, Guo-Qiang Tang28, Takahiro Hiroi29, Derek Sears3, Ilya A. Weinstein7, Alexander S. Vokhmintsev7, Alexei V. Ishchenko7, Phillipe Schmitt-Kopplin30,31, Norbert Hertkorn30, Keisuke Nagao32, Makiko K. Haba32, Mutsumi Komatsu33, and Takashi Mikouchi34 (The Chelyabinsk Airburst Consortium). 1Institute for Dynamics of Geospheres of the Russian Academy of Sciences, Leninsky Prospect 38, Building 1, Moscow, 119334, Russia. 2SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA. 3NASA Ames Research Center, Moffett Field, Mail Stop 245-1, CA 94035, USA. 4Institute of Astronomy of the Russian Academy of Sciences, Pyatnitskaya 48, Moscow, 119017, Russia. 5Department of Theoretical Mechanics, South Ural State University, Lenin Avenue 76, Chelyabinsk, 454080, Russia. 6Chelyabinsk State University, Bratyev Kashirinyh Street 129, Chelyabinsk, 454001, Russia. -
W Numerze: – Wywiad Z Kustoszem Watykańskiej Kolekcji C.D. – Cz¹stki
KWARTALNIK MI£OŒNIKÓW METEORYTÓW METEORYTMETEORYT Nr 3 (63) Wrzesieñ 2007 ISSN 1642-588X W numerze: – wywiad z kustoszem watykañskiej kolekcji c.d. – cz¹stki ze Stardusta a meteorytry – trawienie meteorytów – utwory sp³ywania na Sikhote-Alinach – pseudometeoryty – konferencja w Tucson METEORYT Od redaktora: kwartalnik dla mi³oœników OpóŸnieniami w wydawaniu kolejnych numerów zaczynamy meteorytów dorównywaæ „Meteorite”, którego sierpniowy numer otrzyma³em Wydawca: w paŸdzierniku. Tym razem g³ówn¹ przyczyn¹ by³y k³opoty z moim Olsztyñskie Planetarium komputerem, ale w koñcowej fazie redagowania okaza³o siê tak¿e, i Obserwatorium Astronomiczne ¿e brak materia³u. Musia³em wiêc poczekaæ na mocno opóŸniony Al. Pi³sudskiego 38 „Meteorite”, z którego dorzuci³em dwa teksty. 10-450 Olsztyn tel. (0-89) 533 4951 Przeskok o jeden numer niezupe³nie siê uda³, a zapowiedzi¹ [email protected] dalszych k³opotów jest mi³y sk¹din¹d fakt, ¿e przep³yw materia³ów zacz¹³ byæ dwukierunkowy. W najnowszym numerze „Meteorite” konto: ukaza³ siê artyku³ Marcina Cima³y o Moss z „Meteorytu” 3/2006, 88 1540 1072 2001 5000 3724 0002 a w kolejnym numerze zapowiedziany jest artyku³ o Morasku BOŒ SA O/Olsztyn z „Meteorytu” 4/2006. W rezultacie jednak bêdzie mniej materia³u do Kwartalnik jest dostêpny g³ównie t³umaczenia i trzeba postaraæ siê o dalsze w³asne teksty. Czy mo¿e ktoœ w prenumeracie. Roczna prenu- merata wynosi w 2007 roku 44 z³. chcia³by coœ napisaæ? Zainteresowanych prosimy o wp³a- Z przyjemnoœci¹ odnotowujê, ¿e nabieraj¹ tempa przygotowania cenie tej kwoty na konto wydawcy do kolejnej konferencji meteorytowej, która planowana jest na 18—20 nie zapominaj¹c o podaniu czytel- nego imienia, nazwiska i adresu do kwietnia 2008 r. -
Numerical Modeling of the 2013 Meteorite Entry in Lake Chebarkul, Russia
Nat. Hazards Earth Syst. Sci., 17, 671–683, 2017 www.nat-hazards-earth-syst-sci.net/17/671/2017/ doi:10.5194/nhess-17-671-2017 © Author(s) 2017. CC Attribution 3.0 License. Numerical modeling of the 2013 meteorite entry in Lake Chebarkul, Russia Andrey Kozelkov1,2, Andrey Kurkin2, Efim Pelinovsky2,3, Vadim Kurulin1, and Elena Tyatyushkina1 1Russian Federal Nuclear Center, All-Russian Research Institute of Experimental Physics, Sarov, 607189, Russia 2Nizhny Novgorod State Technical University n. a. R. E. Alekseev, Nizhny Novgorod, 603950, Russia 3Institute of Applied Physics, Nizhny Novgorod, 603950, Russia Correspondence to: Andrey Kurkin ([email protected]) Received: 4 November 2016 – Discussion started: 4 January 2017 Revised: 1 April 2017 – Accepted: 13 April 2017 – Published: 11 May 2017 Abstract. The results of the numerical simulation of possi- Emel’yanenko et al., 2013; Popova et al., 2013; Berngardt et ble hydrodynamic perturbations in Lake Chebarkul (Russia) al., 2013; Gokhberg et al., 2013; Krasnov et al., 2014; Se- as a consequence of the meteorite fall of 2013 (15 Febru- leznev et al., 2013; De Groot-Hedlin and Hedlin, 2014): ary) are presented. The numerical modeling is based on the – the meteorite with a diameter of 16–19 m flew into the Navier–Stokes equations for a two-phase fluid. The results of ◦ the simulation of a meteorite entering the water at an angle earth’s atmosphere at about 20 to the horizon at a ve- ∼ −1 of 20◦ are given. Numerical experiments are carried out both locity of 17–22 km s . when the lake is covered with ice and when it is not. -
The Chelyabinsk Meteorite Fall on February 15, 2013 Attracted Much
46th Lunar and Planetary Science Conference (2015) 2686.pdf MINERALOGY, PETROLOGY, CHRONOLOGY, AND EXPOSURE HISTORY OF THE CHELYABINSK METEORITE AND PARENT BODY. K. Righter1, P. Abell1, D. Agresti2, E. L. Berger3, A.S. Burton1, J.S. Delaney4, M.D. Fries1, E.K. Gibson1, R. Harrington5, G. F. Herzog4, L.P. Keller1, D. Locke6, F. Lindsay4, T.J. McCoy7, R.V. Morris1, K. Nagao8, K. Nakamura-Messenger1, P.B. Niles1, L. Nyquist1, J. Park4, Z.X. Peng9, C.- Y.Shih10, J.I. Simon1, C.C. Swisher, III4, M. Tappa11, and B. Turrin4. 1NASA-JSC, Houston, TX 77058; 2Department of Physics, University of Alabama at Birmingham, Birmingham, AL 35294-1170; 3GeoControl Systems Inc.– Jacobs JETS contract – NASA JSC; 4Rutgers Univ., Wright Labs-Chemistry Dept., Piscataway, NJ; 5UTAS – Jacobs JETS Contract, NASA-JSC; 6HX5 – Jacobs JETS Contract, NASA-JSC; 7Smithsonian Institution, PO Box 37012, MRC 119, Washington, DC; 8Laboratory for Earthquake Chemistry, University of Tokyo, Hongo, Bunkyo- ku, Tokyo 113-0033, Japan; 9Barrios Tech – Jacobs JETS Contract, NASA-JSC; 10Jacobs JETS Contract, NASA- JSC; 11Aerodyne Industries – Jacobs JETS Contract, NASA-JSC. Introduction: The Chelyabinsk meteorite fall in impact melt veins (Figure 2), as compared to on February 15, 2013 attracted much more atten- results of shock experiments [20]. tion worldwide than do most falls [1-3]. A con- Chronology: Portions of light and dark lithol- sortium led by JSC received 3 masses of Chelya- ogies from Chel-101, and the impact melt brecci- binsk (Chel-101, -102, -103) that were collected as (Chel-102 and Chel-103) were prepared and shortly after the fall and handled with care to analyzed for Rb-Sr, Sm-Nd, and Ar-Ar dating. -
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,