DOCSLIB.ORG

Physical Properties of Fireball-Producing Earth-Impacting Meteoroids and Orbit

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Physical Properties of Fireball-Producing Earth-Impacting Meteoroids and Orbit UNIVERSITY OF CALGARY Physical Properties of Fireball-Producing Earth-Impacting Meteoroids and Orbit Determination through Shadow Calibration of the Buzzard Coulee Meteorite Fall by Ellen Palesa Milley A THESIS SUBMITTED TO THE FACULTY OF GRADUATE STUDIES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE DEPARTMENT OF GEOSCIENCE CALGARY, ALBERTA July, 2010 c Ellen Palesa Milley 2010 Library and Archives Bibliothèque et Canada Archives Canada Published Heritage Direction du Branch Patrimoine de l’édition 395 Wellington Street 395, rue Wellington Ottawa ON K1A 0N4 Ottawa ON K1A 0N4 Canada Canada Your file Votre référence ISBN: 978-0-494-69580-7 Our file Notre référence ISBN: 978-0-494-69580-7 NOTICE: AVIS: The author has granted a non- L’auteur a accordé une licence non exclusive exclusive license allowing Library and permettant à la Bibliothèque et Archives Archives Canada to reproduce, Canada de reproduire, publier, archiver, publish, archive, preserve, conserve, sauvegarder, conserver, transmettre au public communicate to the public by par télécommunication ou par l’Internet, prêter, telecommunication or on the Internet, distribuer et vendre des thèses partout dans le loan, distribute and sell theses monde, à des fins commerciales ou autres, sur worldwide, for commercial or non- support microforme, papier, électronique et/ou commercial purposes, in microform, autres formats. paper, electronic and/or any other formats. The author retains copyright L’auteur conserve la propriété du droit d’auteur ownership and moral rights in this et des droits moraux qui protège cette thèse. Ni thesis. Neither the thesis nor la thèse ni des extraits substantiels de celle-ci substantial extracts from it may be ne doivent être imprimés ou autrement printed or otherwise reproduced reproduits sans son autorisation. without the author’s permission. In compliance with the Canadian Conformément à la loi canadienne sur la Privacy Act some supporting forms protection de la vie privée, quelques may have been removed from this formulaires secondaires ont été enlevés de thesis. cette thèse. While these forms may be included Bien que ces formulaires aient inclus dans in the document page count, their la pagination, il n’y aura aucun contenu removal does not represent any loss manquant. of content from the thesis. Abstract The physical properties of the meteoroid population were investigated through combining data from a number of fireball camera networks. PE values, as a measure of meteoroid strength, were calculated and linked with other observational criteria (Tisserand param- eter, meteor shower identification). The historic divisions for fireball types based on the PE criterion were not observed in the large data set, but a correlation with source re- gion was recognized. Meteor showers demonstrated different amounts of variation in PE values potentially related to the materials found in each parent comet. The trajectory and pre-fall orbit for the Buzzard Coulee meteoroid were determined through the calibration of shadows cast by the fireball. The method of using shadows to triangulate a trajectory was developed and evaluated. The best fit trajectory was coupled with an initial velocity of 18.0 km/s to compute the heliocentric orbit. Buzzard Coulee fell from a modestly inclined near-Earth Apollo orbit. It is the 12th fallen meteorite to be associated with an orbit. i Acknowledgements First and foremost I would like to thank Dr. Alan Hildebrand for his experience, guidance and financial support throughout the course of this project. He has given me an incredible number of learning opportunities from the classroom in Geology 699: Meteorites and Asteroids, to travelling the world and meeting other scientists in Prague, Czech Republic. He has been pivotal in the progress of my research project, has extended me invitations for speaking engagements, given me experience working with the media and allowed me to lead some of the meteorite search efforts. It has been an adventure. I am grateful to Dr. Margaret Campbell-Brown for her time and patience working with me throughout the past years. She has provided me with continuous support and supervision throughout my project. She was a wonderful host during my two visits to the University of Western Ontario. I would like to acknowledge Dr. Peter Brown for his time and consistent support throughout my project. In particular, I would like to thank him for the work he did in calibrating Gordon Sarty's all-sky camera to work out an initial velocity for Buzzard Coulee, and in adapting code and running numerous simulations to determine the un- certainties in the trajectory solution. Your knowledge in meteor science is an immense resource, thank you for sharing it with me. Thank you to my examination committee members for taking the time out of their busy schedules to read and review my work. Additionally I would like to thank a number of people for their contributions and guidance. In the Meteor Physics Group at the Uni- versity of Western Ontario: Dr. Wayne Edwards, Sean Kohut and Zbigniew Krzeminski. At Portland State University: Drs. Alex Ruzicka and Melinda Hutson. Thanks to Mike Noble for the effort in taking crucial measurements for the site surveys at camera loca- tions. Rob Cardinal for computer assistance, creating orbit plots and predicting Buzzard ii Coulee's position prior to falling. Jeff Kriz, for driving long hours and staying up late to help take pictures of stars. A special thank you to Lynne Maillet for her computer software assistance, her expertise in mapping and for lending me her camera to take stellar shots. There are hundreds of people who have had an influence over my project, many may not even realize it. Thank you to the landowners, search volunteers, business owners and camera operators in Buzzard Coulee and beyond. I would like to extend my gratitude to video owners for kindly granting me the use of their records: Adam Baxter and the town of Devon, Glenn Lypkie, Alister Ling, Rod and Diana Meger, Ali and Fara Rahmanian, Gordon Sarty, and Rob Tait. Thank you to the landowners, in particular to Al and Jan Mitchell, Ellen and Ian Mitchell, Barb and Elwood Ferguson, for allowing us to trample through their fields in the name of science. A special thank you to Ellen and Ian for their gracious hospitality in hosting our search headquarters and for giving me two rocks that hold a special place in my heart. I am grateful to a number of funding institutions for their support throughout my graduate work: NSERC for a Canada Graduate Scholarship, Alberta Ingenuity Fund for an Incentive Award, the Department of Graduate Studies for two Graduate Research Scholarships, the Canadian Space Agency for a Space Awareness & Learning Grant and to the Graduate Student Association (University of Calgary) for a Conference Grant. Friends and family often seem to be left until the end of the acknowledgements, of course without them I would not be where I am today. Samantha Jones, thank you for showing me how it is all done, you are a role model and a great friend. Thank you to my family for their unwavering support. Bobby, your continuity in my life is a foundation, thank you for your patience. \Equipped with his five senses, man explores the universe around him and calls the adventure Science." | Edwin Hubble, 1889-1953 For my Family. iv v Table of Contents Abstract . i Acknowledgements . ii Table of Contents . v List of Tables . vii List of Figures . viii List of Units and Symbols . xi List of Acronyms and Abbreviations . xiii 1 Introduction . 1 1.1 Comets, Asteroids and Meteors . 1 1.2 Linking Origin and Material . 7 1.2.1 The PE Criterion . 7 1.2.2 The Tisserand Parameter . 9 1.2.3 Meteorites Associated with an Orbit . 9 1.3 The Buzzard Coulee Fall . 15 1.4 Research Project Outline . 15 2 Fireball Network Events . 17 2.1 Historical Overview of Fireball Networks . 17 2.2 Methodology . 21 2.2.1 Calibration, Trajectory and Orbit Derivation . 21 2.2.2 Determining Mass and Calculating the PE Criterion . 23 2.2.3 Combining and Correcting Data from Fireball Networks . 27 2.3 Results and Discussion . 30 2.3.1 PE Value Distributions by Fireball Network . 30 2.3.2 Fireball Strength and Source Region . 34 2.3.3 PE Values of Shower Events . 38 2.3.4 Distribution of Orbital Elements . 41 2.4 Summary and Conclusions . 48 3 The Buzzard Coulee Meteorite Fall . 51 3.1 Introduction to the Buzzard Coulee Event . 51 3.1.1 Naming and Typing of the Meteorite . 54 3.2 Atmospheric Trajectory . 60 3.2.1 Shadow Calibrations . 60 3.2.2 Video Calibrations . 70 3.2.3 Trajectory Results and Discussion . 74 3.2.4 Velocity Results and Discussion . 84 3.3 Pre-Fall Orbit . 89 3.3.1 Discussion . 89 3.4 Summary and Conclusions . 99 Bibliography . 102 A Fireball Networks . 112 B Site Survey Schematics . 115 C Trailside Inn Derivation of Altitude and Azimuth . 119 D MILIG Files . 125 E MORB Files . 150 F Flux of Instrumentally Recorded Meteorite Falls . 153 vi List of Tables 1.1 Meteorites associated with a derived orbit . 12 2.1 Luminous efficiencies published by Ceplecha & McCrosky (1976) . 25 2.2 Luminous efficiencies published by Halliday et al. (1996) . 25 2.3 Breakdown by raw number and raw mass of meteoroid strengths by source region . 37 2.4 Average PE values for meteor shower events . 40 3.1 Buzzard Coulee trajectory solution . 77 3.2 Orbital parameters for the Buzzard Coulee meteoroid . 89 A.1 List of published works used to assemble a data set comprised of MORP, PN and EN events . 112 A.2 Summary of parameters required for the calculation of PE value, Tisserand parameter and the orbital elements .
Load more

Recommended publications
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • Identification of Meteorite Source Regions in the Solar System
    Icarus 311 (2018) 271–287 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Identification of meteorite source regions in the Solar System ∗ Mikael Granvik a,b, , Peter Brown c,d a Department of Physics, P.O. Box 64, 0 0 014 University of Helsinki, Finland b Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Kiruna, Box 848, S-98128, Sweden c Department of Physics and Astronomy, University of Western Ontario, London N6A 3K7, Canada d Centre for Planetary Science and Exploration, University of Western Ontario, London N6A 5B7, Canada a r t i c l e i n f o a b s t r a c t Article history: Over the past decade there has been a large increase in the number of automated camera networks that Received 27 January 2018 monitor the sky for fireballs. One of the goals of these networks is to provide the necessary information Revised 6 April 2018 for linking meteorites to their pre-impact, heliocentric orbits and ultimately to their source regions in the Accepted 13 April 2018 solar system. We re-compute heliocentric orbits for the 25 meteorite falls published to date from original Available online 14 April 2018 data sources. Using these orbits, we constrain their most likely escape routes from the main asteroid belt Keywords: and the cometary region by utilizing a state-of-the-art orbit model of the near-Earth-object population, Meteorites which includes a size-dependence in delivery efficiency. While we find that our general results for escape Meteors routes are comparable to previous work, the role of trajectory measurement uncertainty in escape-route Asteroids identification is explored for the first time.
    [Show full text]
  • Milley 2010.Pdf (10.17Mb)
    University of Calgary PRISM: University of Calgary's Digital Repository Graduate Studies Legacy Theses 2010 Physical Properties of Fireball-Producing Earth-Impacting Meteoroids and Orbit Determination through Shadow Calibration of the Buzzard Coulee Meteorite Fall Milley, Ellen Palesa Milley, E. P. (2010). Physical Properties of Fireball-Producing Earth-Impacting Meteoroids and Orbit Determination through Shadow Calibration of the Buzzard Coulee Meteorite Fall (Unpublished master's thesis). University of Calgary, Calgary, AB. doi:10.11575/PRISM/17766 http://hdl.handle.net/1880/47937 master thesis University of Calgary graduate students retain copyright ownership and moral rights for their thesis. You may use this material in any way that is permitted by the Copyright Act or through licensing that has been assigned to the document. For uses that are not allowable under copyright legislation or licensing, you are required to seek permission. Downloaded from PRISM: https://prism.ucalgary.ca UNIVERSITY OF CALGARY Physical Properties of Fireball-Producing Earth-Impacting Meteoroids and Orbit Determination through Shadow Calibration of the Buzzard Coulee Meteorite Fall by Ellen Palesa Milley A THESIS SUBMITTED TO THE FACULTY OF GRADUATE STUDIES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE DEPARTMENT OF GEOSCIENCE CALGARY, ALBERTA April, 2010 ©c Ellen Palesa Milley 2010 The author of this thesis has granted the University of Calgary a non-exclusive license to reproduce and distribute copies of this thesis to users of the University of Calgary Archives. Copyright remains with the author. Theses and dissertations available in the University of Calgary Institutional Repository are solely for the purpose of private study and research.
    [Show full text]
  • Lev A. Muravyev , Viktor I. Grokhovsky
    The Chrono List of Bad Meteorites Harmful № Date Name Place Type Fall Description Source 1Ural Federal University, specimen 1,2 Lombardia, Doubtful 2 1 04.09.1511 Crema shwr several killed birds, sheep, and a man (dbt) [3, 7] Lev A. Muravyev , Institute of Geophysics Ural Branch of RAS, Italy meteorite Doubtful 2 04.09.1654 Milan Italy {?} - killed a monk (dbt) [3, 7] 1 Ekaterinburg, Russia; meteorite Aquitaine, crushed cottage, killed farmer and Viktor I. Grokhovsky 3 24.07.1790 Barbotan H5 shwr - [1, 10] [email protected], [email protected] France some cattle (dbt) Uttar Pradesh, [7, 9, Abstract. The problem of the asteroid-comet hazard is now being 4 19.12.1798 Benares (a) LL4 shwr 0,9 kg building India 10] actively discussed, because the consequences of the fall of large cosmic Bayern, 5 13.12.1803 Mässing Howardite U - building struck [1, 10] bodies on the earth can be catastrophic and affect the survival of Germany humanity and all living things. Fragments of smaller celestial bodies - Moscow, 6 05.09.1812 Borodino H5 U 0,5 kg observed by a soldier on guard [7] meteorites, fall to the earth much more often, and they can also emanate Russia a certain danger. In several papers that were published about 20 years Rajasthan, Doubtful killed a men and injured a women 7 16.01.1825 Oriang {?} - [3, 7] ago, attempts were made to compile a list of events related to the India meteorite (dbt) Uttar Pradesh, [3, 7, 9, damage caused by meteorites falling from the sky.
    [Show full text]
  • The Fall of the Peekskill Meteorite: Video Observations, Atmospheric
    The Fall of the Peekskill Meteorite: Video Observaüons, Atmospheric Path, Fragmentation Record and Orbit. M. Beech 1, P. Brown 2, R. L. Hawkes3, Z. Ceplecha4, K. Mossman3, and G. Wetherill5. 1 Astronomy Department, The University of Western Ontario, London, Ontario, Canada. 2 Physics Department, The University of Western Ontario, London, Ontario, Canada. 3 Department of Physics, Engineering and Geology, Mount Allison University, Sackville, New Brunswick, Canada. 40ndrejov Observatory, Astronomieal Institute of the Academy of Sciences of the Czech Republic, Ondrejov, Czech Republic. 5 Camegie lnsütute of Washington, Department of Terrestrial Magneüsm, 5241 Broad Branch Road, Washington, D. C., U.S.A. Abstract A general overview of the events surrounding the fall of the Peekskill meteorite is presented. Earth, Moon, and Planets 68: 189-197, 1995. © 1995 Kluwer Academic Publlshers. Printed in the Netherlands. 190 1. Introduetion: The events surrounding the fall of the Peekskill meteorite on October 9th, 1992 are quite remarkable. Not only did the meteorite announce its arrival by hitting a parked car in suburban Peekskill, N.Y., but the fireball that preceded the fall of the meteorite was videographed by at least 16 independent videographers. Eye-witness accounts indicate that the fireball associated with the Peekskill meteodte first appeared over West Virginia at 23:48 UT (±1 min.). The fireball, which traveled in an approximately northeasterly direction, had a pronounced greenish colour, and attained an estimated peak visual magnitude of -13 (comparable to the Full Moon). During a luminous flight time that exceeded 40 seconds the fireball covered a ground path of some 700 to 800 km (Brown et al., 1994).
    [Show full text]
  • Fersman Mineralogical Museum of the Russian Academy of Sciences (FMM)
    Table 1. The list of meteorites in the collections of the Fersman Mineralogical Museum of the Russian Academy of Sciences (FMM). Leninskiy prospect 18 korpus 2, Moscow, Russia, 119071. Pieces Year Mass in Indication Meteorite Country Type in found FMM in MB FMM Seymchan Russia 1967 Pallasite, PMG 500 kg 9 43 Kunya-Urgench Turkmenistan 1998 H5 402 g 2 83 Sikhote-Alin Russia 1947 Iron, IIAB 1370 g 2 Sayh Al Uhaymir 067 Oman 2000 L5-6 S1-2,W2 63 g 1 85 Ozernoe Russia 1983 L6 75 g 1 66 Gujba Nigeria 1984 Cba 2..8 g 1 85 Dar al Gani 400 Libya 1998 Lunar (anorth) 0.37 g 1 82 Dhofar 935 Oman 2002 H5S3W3 96 g 1 88 Dhofar 007 Oman 1999 Eucrite-cm 31.5 g 1 84 Muonionalusta Sweden 1906 Iron, IVA 561 g 3 Omolon Russia 1967 Pallasite, PMG 1,2 g 1 72 Peekskill USA 1992 H6 1,1 g 1 75 Gibeon Namibia 1836 Iron, IVA 120 g 2 36 Potter USA 1941 L6 103.8g 1 Jiddat Al Harrasis 020 Oman 2000 L6 598 gr 2 85 Canyon Diablo USA 1891 Iron, IAB-MG 329 gr 1 33 Gold Basin USA 1995 LA 101 g 1 82 Campo del Cielo Argentina 1576 Iron, IAB-MG 2550 g 4 36 Dronino Russia 2000 Iron, ungrouped 22 g 1 88 Morasko Poland 1914 Iron, IAB-MG 164 g 1 Jiddat al Harasis 055 Oman 2004 L4-5 132 g 1 88 Tamdakht Morocco 2008 H5 18 gr 1 Holbrook USA 1912 L/LL5 2,9g 1 El Hammami Mauritani 1997 H5 19,8g 1 82 Gao-Guenie Burkina Faso 1960 H5 18.7 g 1 83 Sulagiri India 2008 LL6 2.9g 1 96 Gebel Kamil Egypt 2009 Iron ungrouped 95 g 2 98 Uruacu Brazil 1992 Iron, IAB-MG 330g 1 86 NWA 859 (Taza) NWA 2001 Iron ungrouped 18,9g 1 86 Dhofar 224 Oman 2001 H4 33g 1 86 Kharabali Russia 2001 H5 85g 2 102 Chelyabinsk
    [Show full text]
  • Meteorite Auction - Macovich Collection
    Meteorite Auction - Macovich Collection HOME l INTRO TO MACOVICH l METEORITES FOR SALE l MEDIA INFO l CONTACT US THE MACOVICH METEORITE AUCTION Sunday February 9, 2003 10:30 A.M. at the InnSuites — Courtyard Terrace 475 North Granada, Tucson (520) 622-3000 Previews & In-person Registration February 1 – February 9 (10:30AM – 6 PM) February 9 (9:30AM – 10:30AM) Room 404 at the InnSuites Hotel AUCTION NOTES You must register to participate. Dimensions of lots are approximate. There is a 12.5% buyer's commission on all lots. Low and high estimates are merely a guideline. Witnessed falls are denoted by an asterisk. A bullet to the left of the lot number indicates that the specimen carries a reserve. Meteorites of a more decorative or sculptural nature are designated by a green box around the lot number. LOT NAME DATE OF WEIGHT & TKW LOCALITY DESCRIPTION ESTIMATE # TYPE FALL/FIND DIMENSIONS CLICK ON METEORITE NAME TO VIEW IMAGE AND DESCRIPTION Naiman* Naiman Cnty, Encrusted fragment of an extremely difficult to obtain meteorite; 12.55 g 1 May/26/1982 1.05 Kg $150 – $250 L6 Mongolia Purple Mountain Observatory provenance 27 x 28 x 14 Kilabo* Complete specimen of Earth's most recent meteorite recovery 83.20 g 2 July/21/2002 ~24 Kg Hadejia, Nigeria $600 – $750 LL6 to date; ~90% fusion crust 48 x 35 x 35 Highly brecciated thin quarter slice of this much sought–after Honolulu* 1.99 g 3 Sep/27/1825 ~3 Kg Oahu, Hawaii meteorite; with fusion crust; Finnish Geological Museum $250 – $350 L5 27 x 21 x 1 provenance Partial slice; the most famous meteorite/auto
    [Show full text]
  • Small Near-Earth Asteroids As a Source of Meteorites
    Small Near-Earth Asteroids as a Source of Meteorites Jiří Borovička and Pavel Spurný Astronomical Institute of the Czech Academy of Sciences Peter Brown University of Western Ontario __________________________________________________________________________ Small asteroids intersecting Earth’s orbit can deliver extraterrestrial rocks to the Earth, called meteorites. This process is accompanied by a luminous phenomena in the atmosphere, called bolides or fireballs. Observations of bolides provide pre-atmospheric orbits of meteorites, physical and chemical properties of small asteroids, and the flux (i.e. frequency of impacts) of bodies at the Earth in the centimeter to decameter size range. In this chapter we explain the processes occurring during the penetration of cosmic bodies through the atmosphere and review the methods of bolide observations. We compile available data on the fireballs associated with 22 instrumentally observed meteorite falls. Among them are the heterogeneous falls Almahata Sitta (2008 TC3) and Benešov, which revolutionized our view on the structure and composition of small asteroids, the Příbram-Neuschwanstein orbital pair, carbonaceous chondrite meteorites with orbits on the asteroid-comet boundary, and the Chelyabinsk fall, which produced a damaging blast wave. While most meteoroids disrupt into fragments during atmospheric flight, the Carancas meteoroid remained nearly intact and caused a crater-forming explosion on the ground. 1. INTRODUCTION Well before the first asteroid was discovered, people unknowingly had asteroid samples in their hands. Could stones fall from the sky? For many centuries, the official answer was: NO. Only at the end of the 18th century and the beginning of the 19th century did the evidence that rocks did fall from the sky become so overwhelming that this fact was accepted by the scientific community.
    [Show full text]
  • Minerals in Meteorites
    APPENDIX 1 Minerals in Meteorites Minerals make up the hard parts of our world and the Solar System. They are the building blocks of all rocks and all meteorites. Approximately 4,000 minerals have been identified so far, and of these, ~280 are found in meteorites. In 1802 only three minerals had been identified in meteorites. But beginning in the 1960s when only 40–50 minerals were known in meteorites, the discovery rate greatly increased due to impressive new analytic tools and techniques. In addition, an increasing number of different meteorites with new minerals were being discovered. What is a mineral? The International Mineralogical Association defines a mineral as a chemical element or chemical compound that is normally crystalline and that has been formed as a result of geological process. Earth has an enormously wide range of geologic processes that have allowed nearly all the naturally occurring chemical elements to participate in making minerals. A limited range of processes and some very unearthly processes formed the minerals of meteorites in the earliest history of our solar system. The abundance of chemical elements in the early solar system follows a general pattern: the lighter elements are most abundant, and the heavier elements are least abundant. The miner- als made from these elements follow roughly the same pattern; the most abundant minerals are composed of the lighter elements. Table A.1 shows the 18 most abundant elements in the solar system. It seems amazing that the abundant minerals of meteorites are composed of only eight or so of these elements: oxygen (O), silicon (Si), magnesium (Mg), iron (Fe), aluminum (Al), calcium (Ca), sodium (Na) and potas- sium (K).
    [Show full text]
  • Meteorite Mineralogy Alan Rubin , Chi Ma Index More Information
    Cambridge University Press 978-1-108-48452-7 — Meteorite Mineralogy Alan Rubin , Chi Ma Index More Information Index 2I/Borisov, 104, See interstellar interloper alabandite, 70, 96, 115, 142–143, 151, 170, 174, 177, 181, 187, 189, 306 Abbott. See meteorite Alais. See meteorite Abee. See meteorite Albareto. See meteorite Acapulco. See meteorite Albin. See meteorite acapulcoites, 107, 173, 179, 291, 303, Al-Biruni, 3 309, 314 albite, 68, 70, 72, 76, 78, 87, 92, 98, 136–137, 139, accretion, 238, 260, 292, 347, 365 144, 152, 155, 157–158, 162, 171, 175, 177–178, acetylene, 230 189–190, 200, 205–206, 226, 243, 255–257, 261, Acfer 059. See meteorite 272, 279, 295, 306, 309, 347 Acfer 094. See meteorite albite twinning, 68 Acfer 097. See meteorite Aldrin, Buzz, 330 achondrites, 101, 106–108, 150, 171, 175, 178–179, Aletai. See meteorite 182, 226, 253, 283, 291, 294, 303, 309–310, 318, ALH 77307. See meteorite 350, 368, 374 ALH 78091. See meteorite acute bisectrix, 90 ALH 78113. See meteorite adamite, 83 ALH 81005. See meteorite addibischoffite, 116, 167 ALH 82130. See meteorite Adelaide. See meteorite ALH 83009. See meteorite Adhi Kot. See meteorite ALH 83014. See meteorite Admire. See meteorite ALH 83015. See meteorite adrianite, 117, 134, 167, 268 ALH 83108. See meteorite aerogel, 234 ALH 84001. See meteorite Aeschylus, 6 ALH 84028. See meteorite agate, 2 ALH 85085. See meteorite AGB stars. See asymptotic giant branch stars ALH 85151. See meteorite agglutinate, 201, 212, 224, 279, 301–302, 308 ALHA76004. See meteorite Agpalilik. See Cape York ALHA77005.
    [Show full text]