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Astronomy 150: Killer Skies Lecture 5, January 27
Astronomy 150: Killer Skies Lecture 5, January 27 Last time: began Astro Threat I: Impacts Today: Meteors and Asteroids Homework: ‣ HW 1 due today, but allowing submission up until next Monday. ‣ HW 2 posted today, due next Friday at the start of class http://epod.usra.edu/blog/2011/01/fireball-breakup.html http://epod.usra.edu/blog/2011/05/willamette-meteorite.html Friday, January 27, 2012 Register your i>clicker Go to link on class web page to register your i>clicker ‣ Register with first part of your @illinois.edu email (NetID) If you can’t read your i>clicker ID ‣ Go the Illini bookstore bag-check counter ‣ Vote with your i>clicker ‣ Clicker ID will be displayed on the base unit https://online-s.physics.uiuc.edu/cgi/courses/shell/iclicker.pl Friday, January 27, 2012 Register your i>clicker Go to link on class web page to register your i>clicker ‣ Register with first part of your @illinois.edu email (NetID) If you can’t read your i>clicker ID ‣ Go the Illini bookstore bag-check counter ‣ Vote with your i>clicker ‣ Clicker ID will be displayed on the base unit https://online-s.physics.uiuc.edu/cgi/courses/shell/iclicker.pl Friday, January 27, 2012 Planetarium Session Purpose: ‣ To help you understand the motions of the sky Dates: 1/30, 1/31, 2/2, 2/6, 2/7, 2/8 @ Staerkel Planetarium, Parkland College ‣ Show starts at 7pm, runs ~80 minutes ‣ $3 door charge, please bring exact change Report due Feb 24th in class ‣ Details on class website ‣ Attach ticket from the show to your report Reserve a seat online ‣ Link to reservation site on class website Friday, January 27, 2012 Fireballs Since most meteors are from small objects, they burn up before they hit the ground. -
Disequilibrium Melting and Melt Migration Driven by Impacts: Implications for Rapid Planetesimal Core Formation
Available online at www.sciencedirect.com Geochimica et Cosmochimica Acta 100 (2013) 41–59 www.elsevier.com/locate/gca Disequilibrium melting and melt migration driven by impacts: Implications for rapid planetesimal core formation Andrew G. Tomkins ⇑, Roberto F. Weinberg, Bruce F. Schaefer 1, Andrew Langendam School of Geosciences, P.O. Box 28E, Monash University, Melbourne, Victoria 3800, Australia Received 20 January 2012; accepted in revised form 24 September 2012; available online 12 October 2012 Abstract The e182W ages of magmatic iron meteorites are largely within error of the oldest solar system particles, apparently requir- ing a mechanism for segregation of metals to the cores of planetesimals within 1.5 million years of initial condensation. Cur- rently favoured models involve equilibrium melting and gravitational segregation in a static, quiescent environment, which requires very high early heat production in small bodies via decay of short-lived radionuclides. However, the rapid accretion needed to do this implies a violent early accretionary history, raising the question of whether attainment of equilibrium is a valid assumption. Since our use of the Hf–W isotopic system is predicated on achievement of chemical equilibrium during core formation, our understanding of the timing of this key early solar system process is dependent on our knowledge of the seg- regation mechanism. Here, we investigate impact-related textures and microstructures in chondritic meteorites, and show that impact-generated deformation promoted separation of liquid FeNi into enlarged sulfide-depleted accumulations, and that this happened under conditions of thermochemical disequilibrium. These observations imply that similar enlarged metal accumu- lations developed as the earliest planetesimals grew by rapid collisional accretion. -
The History of the Hoba Meteorite III: Known and Loved by All
the hoba meteorite The History of the Hoba Meteorite III: Known and loved by all ... P E Spargo Department of Physics, University of Cape Town, Rondebosch 7701, South Africa [email protected] In spite of its remote location in the However, apart from Luyten’s very brief then little-visited and almost unknown note in the Harvard College Observatory territory of South-West Africa (Namibia Bulletin (Luyten, 1929a, reproduced in today), we saw previously (Spargo facsimile in Fig. 8 in the second of this 2008b) that the second decade of the series of articles) and his short, largely great meteorite’s life opened with its descriptive articles in the South African existence being relatively widely known Journal of Science (Luyten 1929b) and to the public in South Africa and the Popular Astronomy (Luyten, 1930), noth- United States. This was as a result of ing of serious scientific import had been articles in Die Volksblad (Bloemfon- published. tein), The Cape Times (Cape Town), The Star (Johannesburg) and The New York It will be recalled, however, that on 5 Times1. There were also brief notes in September 1929 the meteorite had been Die Sterne (R.H., 1930), the popular visited by a small party of geologists who German astronomical magazine, which were on an excursion to Southwest Africa at least alerted German astronomers following the International Geological to its existence, and the Zeitschrift für Congress, which had held its XV Session Praktische Geologie (Schneiderhöhn, in South Africa in July and August of that 1929) performing a similar function for year. -
An Evaluation of the Palladium-Silver Isotope Systematics in the Oldest Differentiated Planetesimal: Beyond Shock
43rd Lunar and Planetary Science Conference (2012) 1116.pdf AN EVALUATION OF THE PALLADIUM-SILVER ISOTOPE SYSTEMATICS IN THE OLDEST DIFFERENTIATED PLANETESIMAL: BEYOND SHOCK. M.F. Horan1, R.W. Carlson1,and J. Blichert-Toft2 Department of Terrestrial Magnetism, Carnegie Institution of Washington (5241 Broad Branch Road NW, Washing- ton DC 20015. [email protected]), 2Ecole Normale Supérieure de Lyon, Université Claude Bernard Lyon 1 and CNRS (69007 Lyon, France). Introduction: Troilite from Muonionalusta (iron Troilite from slab 1 contained 5.612 ng/g Ag with meteorite group IVA) gives the oldest absolute age yet 107Ag/109Ag of 1.127±0.002, and 0.780±0.002 ng/g Pd, measured for a differentiated planetesimal corresponding to 108Pd/109Ag of 0.05946 ±0.00010. (4565.3±0.1 Ma) which suggests that the IVA parent HCl-insoluble inclusions (probably schreibersite) with- body accreted, differentiated, and cooled within 2-3 in this troilite yielded 1.758±0.006 ng/g Ag with Ma after CAI formation [1]. The aim of this study is to 107Ag/109Ag of 1.130±0.002, and 5168±10 ng/g Pd, use the quick evolution and volatile-depleted (high corresponding to 108Pd/109Ag of 1691±8. Troilite from Pd/Ag) composition of IVA irons to better constrain slab 2 contained 11.75±0.04 ng/g Ag and had a the initial Solar System abundance of 107Pd ( 107Pd 107Ag/109Ag ratio of 1.0833±0.0004 [6]. The Pd con- 107 Ag with t1/2 = 6.5 Ma). Most Pd/Ag ages have been centration was 0.291±0.1 ng/g corresponding to referenced to 107Pd/108Pd = (2.40±0.05) x 10-5 obtained 108Pd/109Ag of 13.9±0.1. -
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. -
Ron Hartman and the Lucerne Valley Meteorites by Robert Verish Ron Hartman and the Lucerne Valley Meteorites
Meteorite Times Magazine Contents by Editor 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 Meteorite Calendar by Anne Black Meteorite of the Month by Editor 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 2002–2011 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. -
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. -
N Arieuican%Mllsellm
n ARieuican%Mllsellm PUBLISHED BY THE AMERICAN MUSEUM OF NATURAL HISTORY CENTRAL PARK WEST AT 79TH STREET, NEW YORK 24, N.Y. NUMBER 2I63 DECEMBER I9, I963 The Pallasites BY BRIAN MASON' INTRODUCTION The pallasites are a comparatively rare type of meteorite, but are remarkable in several respects. Historically, it was a pallasite for which an extraterrestrial origin was first postulated because of its unique compositional and structural features. The Krasnoyarsk pallasite was discovered in 1749 about 150 miles south of Krasnoyarsk, and seen by P. S. Pallas in 1772, who recognized these unique features and arranged for its removal to the Academy of Sciences in St. Petersburg. Chladni (1794) examined it and concluded it must have come from beyond the earth, at a time when the scientific community did not accept the reality of stones falling from the sky. Compositionally, the combination of olivine and nickel-iron in subequal amounts clearly distinguishes the pallasites from all other groups of meteorites, and the remarkable juxtaposition of a comparatively light silicate mineral and heavy metal poses a nice problem of origin. Several theories of the internal structure of the earth have postulated the presence of a pallasitic layer to account for the geophysical data. No apology is therefore required for an attempt to provide a comprehensive account of this remarkable group of meteorites. Some 40 pallasites are known, of which only two, Marjalahti and Zaisho, were seen to fall (table 1). Of these, some may be portions of a single meteorite. It has been suggested that the pallasite found in Indian mounds at Anderson, Ohio, may be fragments of the Brenham meteorite, I Chairman, Department of Mineralogy, the American Museum of Natural History. -
Richardton and New Leipzig Meteorites Returning to North Dakota by Ed Murphy on the Evening of June 30, 1918 (About 10:00 P.M
Richardton and New Leipzig Meteorites Returning to North Dakota By Ed Murphy On the evening of June 30, 1918 (about 10:00 p.m. he received from Muggli, to George Merrill, Head Curator of mountain time), the Richardton meteorite fell to earth on either Geology at the Smithsonian. Merrill verified it was a stony side of ND Highway 8 about equidistance between the towns meteorite, but interestingly enough noted that it was quite of Richardton and Mott (fig. 1). The fireball of the meteoroid, weathered and that it probably belonged to an earlier fall, as it raced across the sky, was witnessed over an area of at that is, it was not the Richardton meteorite. least 18,000 square miles (fig. 2). A witness who was 130 miles to the southwest said, “As it came down, it illuminated Leonard was attempting to purchase specimens of the the landscape to almost the brilliancy of sunlight.” Witnesses Richardton meteorite when he received a letter dated closer to the fall area likened the sound of the meteoroid to an November 10, 1918 from T.T. Quirke. Quirke, a professor of “airship” or motorcycle. The 200-pound meteoroid broke geology at the University of Minnesota, had been sent out by into at least 200 pieces perhaps at a height of 60 miles above that department to investigate the fall. There is evidence that the earth. The sound of the breakup was said to have been a John Muggli contacted Quirke when he was unable to reach “fearful and terrifying noise,” “a deep tone thundering,” “a violent Leonard. -
Investigate the History of the Solar System
ARTHUR ROSS HALL OF METEORITES Grades 9-12 Investigate the History of the Solar System Overview Correlations to Standards Students will learn about meteorites and how scientists use these space rocks NY ES4 1.2C: Our solar system formed to investigate how the solar system formed and evolved. about five billion years ago from a giant cloud of gas and debris. Gravity caused • Before Your Visit: Students will complete a formative assessment probe, Earth and other planets to become and read and discuss a text about how and why scientists study meteorites. layered according to density differences in their materials. • During Your Visit: In the Arthur Ross Hall of Meteorites, students will observe meteorite samples to uncover the story of the formation and evolution of the solar system. Then, in the Gottesman Hall of Planet Earth, students will learn more about the formation of the Earth-Moon system, and search for impact craters on Earth and the Moon. • Back in the Classroom: Students will produce an illustrated text that describes the history of the solar system and explains how meteorites help scientists uncover this history. Background for Educators Meteorites are space debris that has fallen to Earth. They’re called meteoroids when still in deep space, meteors (or “shooting stars”) when falling through the atmosphere, and meteorites after they land on Earth. Meteorites range in size from microscopic to kilometers in diameter. They all originate inside our solar system. Most are fragments of small rocky and metallic bodies that broke apart long ago and orbit the Sun in the asteroid belt between Mars and Jupiter. -
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. -
Trace Element Chemistry of Cumulus Ridge 04071 Pallasite with Implications for Main Group Pallasites
Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites Item Type Article; text Authors Danielson, L. R.; Righter, K.; Humayun, M. Citation Danielson, L. R., Righter, K., & Humayun, M. (2009). Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites. Meteoritics & Planetary Science, 44(7), 1019-1032. DOI 10.1111/j.1945-5100.2009.tb00785.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 23/09/2021 14:17:54 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656592 Meteoritics & Planetary Science 44, Nr 7, 1019–1032 (2009) Abstract available online at http://meteoritics.org Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites Lisa R. DANIELSON1*, Kevin RIGHTER2, and Munir HUMAYUN3 1Mailcode JE23, NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas 77058, USA 2Mailcode KT, NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas 77058, USA 3National High Magnetic Field Laboratory and Department of Geological Sciences, Florida State University, Tallahassee, Florida 32310, USA *Corresponding author. E-mail: [email protected] (Received 06 November 2008; revision accepted 11 May 2009) Abstract–Pallasites have long been thought to represent samples from the metallic core–silicate mantle boundary of a small asteroid-sized body, with as many as ten different parent bodies recognized recently. This report focuses on the description, classification, and petrogenetic history of pallasite Cumulus Ridge (CMS) 04071 using electron microscopy and laser ablation ICP-MS.