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Calcium Isotopes in Natural and Experimental Carbonated Silicate Melts
Western University Scholarship@Western Electronic Thesis and Dissertation Repository 2-27-2018 2:30 PM Calcium Isotopes in Natural and Experimental Carbonated Silicate Melts Matthew Maloney The University of Western Ontario Supervisor Bouvier, Audrey The University of Western Ontario Co-Supervisor Withers, Tony The University of Western Ontario Graduate Program in Geology A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Matthew Maloney 2018 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Geochemistry Commons Recommended Citation Maloney, Matthew, "Calcium Isotopes in Natural and Experimental Carbonated Silicate Melts" (2018). Electronic Thesis and Dissertation Repository. 5256. https://ir.lib.uwo.ca/etd/5256 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. Abstract The calcium stable isotopic compositions of mantle-sourced rocks and minerals were investigated to better understand the carbon cycle in the Earth’s mantle. Bulk carbonatites and kimberlites were analyzed to identify a geochemical signature of carbonatite magmatism, while inter-mineral fractionation was measured in co-existing Ca-bearing carbonate and silicate minerals. Bulk samples show a range of composition deviating from the bulk silicate Earth δ44/40Ca composition indicating signatures of magmatic processes or marine carbonate addition 44/40 to source materials. Δ Cacarbonate-silicate values range from -0.55‰ to +1.82‰ and positively correlate with Ca/Mg ratios in pyroxenes. -
Asteroid Regolith Weathering: a Large-Scale Observational Investigation
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved. -
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Xb1oxfitateie'ian%Mlseltm PUBLISHED BY THE AMERICAN MUSEUM OF NATURAL HISTORY CENTRAL PARK WEST AT 79TH STREET, NEW YORK 24, N.Y. NUMBER 2 I 90 SEPTEMBER IO, I964 The Meteorite and Tektite Collection of the American Museum of Natural History BY BRIAN MASON' INTRODUCTION The first meteorite received by the American Museum of Natural History was a 46-gram piece of the Searsmont chondrite, presented by G. M. Brainerd of Rockland, Maine, in 1872. For some years the col- lection grew very slowly. Hovey (1896) published the first catalogue, in which he enumerated 55 pieces representing 26 different meteorites. However, the status of the collection was radically changed in 1900 with the acquisition of the Bement collection of minerals, through the gener- osity ofJ. Pierpont Morgan. Besides some 12,000 mineral specimens, the Bement collection contained 580 meteorites, representing nearly 500 different falls and finds. This acquisition established the meteorite col- lection of this museum as one of the great collections of the world, a situation that has been maintained by more recent additions. Some of the more notable additions may be briefly noted. In 1904 three Cape York irons, brought from Greenland in 1897 by R. E. Peary, were deposited in the museum. These are known as "Ahnighito" or "The Tent," "The Woman," and "The Dog" (fig. 1). "Ahnighito," the largest of the three, is approximately 11 feet long, 7 feet high, and 6 feet thick. Various estimates of its weight, ranging from 30 to 80 tons, have been published. Thanks to the Toledo Scale Company it was mounted 1 Chairman, Department of Mineralogy, the American Museum of Natural History. -
Link Between the Potentially Hazardous Asteroid (86039) 1999 NC43 and the Chelyabinsk Meteoroid Tenuous ⇑ Vishnu Reddy A,1, , David Vokrouhlicky´ B, William F
Icarus 252 (2015) 129–143 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Link between the potentially hazardous Asteroid (86039) 1999 NC43 and the Chelyabinsk meteoroid tenuous ⇑ Vishnu Reddy a,1, , David Vokrouhlicky´ b, William F. Bottke c, Petr Pravec d, Juan A. Sanchez a,1, Bruce L. Gary e, Rachel Klima f, Edward A. Cloutis g, Adrián Galád d, Tan Thiam Guan h, Kamil Hornoch d, Matthew R.M. Izawa g, Peter Kušnirák d, Lucille Le Corre a,1, Paul Mann g, Nicholas Moskovitz i,1, Brian Skiff i, Jan Vraštil b a Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA b Institute of Astronomy, Charles University, V Holešovicˇkách 2, CZ-18000 Prague, Czech Republic c Southwest Research Institute, 1050 Walnut St, Suite 300, Boulder, CO 80302, USA d Astronomical Institute, Academy of Sciences of the Czech Republic, Fricˇova 1, CZ-25165 Ondrˇejov, Czech Republic e Hereford Arizona Observatory, Hereford, AZ 85615, USA f Johns Hopkins University/Applied Physics Laboratory, Laurel, MD, USA g Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, Manitoba R3B 2E9, Canada h Perth Exoplanet Survey Telescope, 20 Lisle St, Mount Claremont, WA 6010, Australia i Lowell Observatory, 1400 W Mars Hill Road, Flagstaff, AZ 86001, USA article info abstract Article history: We explored the statistical and compositional link between Chelyabinsk meteoroid and potentially haz- Received 31 July 2014 ardous Asteroid (86039) 1999 NC43 to investigate their proposed relation proposed by Borovicˇka et al. Revised 17 December 2014 (Borovicˇka, J., et al. [2013]. Nature 503, 235–237). -
February 16-22, 2020
8# Ice & Stone 2020 Week 8: February 16-22, 2020 Presented by The Earthrise Institute This week in history FEBRUARY 16 17 18 19 20 21 22 FEBRUARY 17, 1930: A bright meteor appears in the sky above the midwestern U.S. and falls to the ground near Paragould, Arkansas. With a total mass of 370 kg, the Paragould meteorite, a stony chondrite, is the second- largest meteorite fall seen from and recovered in North America. FEBRUARY 17, 1996: The Near-Earth Asteroid Rendezvous (NEAR) spacecraft – later renamed NEAR Shoemaker after renowned planetary geologist Eugene Shoemaker – is launched from Cape Canaveral, Florida. After passing by the main-belt asteroid (253) Mathilde in June 1997 and the near-Earth asteroid (433) Eros in late 1998, NEAR Shoemaker returned to Eros in February 2000 and went into orbit around it, and one year later successfully soft-landed onto Eros’ surface. The NEAR Shoemaker mission was covered in a previous “Special Topics” presentation. FEBRUARY 16 17 18 19 20 21 22 FEBRUARY 18, 1930: Clyde Tombaugh at Lowell Observatory in Arizona discovers Pluto while examining photographs he had taken in late January. Pluto is the subject of a future “Special Topics” presentation. FEBRUARY 18, 1948: A bright meteor appears over the midwestern U.S. and drops a large shower of meteorites over parts of Kansas and Nebraska. The Norton County meteorite, as this has been called, has a total mass of 1070 kg and is the largest meteorite fall seen from and recovered in North America. FEBRUARY 18, 1991: Rob McNaught at Siding Spring Observatory in New South Wales discovers the apparent “asteroid” now known as (5335) Damocles. -
The Stubenberg Meteorite—An LL6 Chondrite Fragmental Breccia Recovered Soon After Precise Prediction of the Strewn field
Meteoritics & Planetary Science 1–21 (2017) doi: 10.1111/maps.12883 The Stubenberg meteorite—An LL6 chondrite fragmental breccia recovered soon after precise prediction of the strewn field Addi BISCHOFF1,* , Jean-Alix BARRAT2, Kerstin BAUER3, Christoph BURKHARDT1, Henner BUSEMANN3 , Samuel EBERT1, Michael GONSIOR4, Janina HAKENMULLER€ 5, Jakub HALODA6, Dennis HARRIES7, Dieter HEINLEIN8, Harald HIESINGER1, Rupert HOCHLEITNER9, Viktor HOFFMANN10, Melanie KALIWODA9, Matthias LAUBENSTEIN11, Colin MADEN3, Matthias M. M. MEIER3 , Andreas MORLOK1, Andreas PACK12, Alexander RUF13,14, Philippe SCHMITT-KOPPLIN13,14, Maria SCHONB€ ACHLER€ 3, Robert C. J. STEELE3, Pavel SPURNY 15, and Karl WIMMER16 1Institut fur€ Planetologie, Westfalische€ Wilhelms-Universitat€ Munster,€ Wilhelm-Klemm Str. 10, Munster€ D-48149, Germany 2Universite de Bretagne Occidentale, Institut Universitaire Europeen de la Mer, Place Nicolas Copernic, Plouzane Cedex F-29280, France 3ETH Zurich,€ Institut fu¨ r Geochemie und Petrologie, Clausiusstrasse 25, Zurich€ CH-8092, Switzerland 4University of Maryland, Center for Environmental Science, Chesapeake Biological Laboratory, 146 Williams Street, Solomons, Maryland 20688, USA 5Max-Planck-Institut fur€ Kernphysik, Saupfercheckweg 1, Heidelberg D-69117, Germany 6Czech Geological Survey, Geologicka 6, Praha 5 CZ-152 00, Czech Republic 7Institut fur€ Geowissenschaften, Friedrich-Schiller-Universitat€ Jena, Carl-Zeiss-Promenade 10, Jena D-07745, Germany 8German Fireball Network, Lilienstraße 3, Augsburg D-86156, Germany 9Mineralogische -
Nature and Origins of Meteoritic Breccias 679
Bischoff et al.: Nature and Origins of Meteoritic Breccias 679 Nature and Origins of Meteoritic Breccias Addi Bischoff Westfälische Wilhelms-Universität Münster Edward R. D. Scott University of Hawai‘i Knut Metzler Westfälische Wilhelms-Universität Münster Cyrena A. Goodrich University of Hawai‘i Meteorite breccias provide information about impact processes on planetary bodies, their collisional evolution, and their structure. Fragmental and regolith breccias are abundant in both differentiated and chondritic meteorite groups and together with rarer impact-melt rocks pro- vide constraints on cratering events and catastrophic impacts on asteroids. These breccias also constrain the stratigraphy of differentiated and chondritic asteroids and the relative abundance of different rock types among projectiles. Accretional chondritic breccias formed at low impact speeds (typically tens or hundreds of meters per second), while other breccias reflect hyper- velocity impacts at higher speeds (~5 km/s) after asteroidal orbits were dynamically excited. Iron and stony-iron meteorite breccias only formed, when their parent bodies were partly molten. Polymict fragmental breccias and regolith breccias in some meteorite groups contain unique types of clasts that do not occur as individual meteorites in our collections. For example, ureilite breccias contain feldspathic clasts from the ureilite parent body as well as carbonaceous chon- dritic projectile material. Such clasts provide new rock types from both unsampled parent bod- ies and unsampled parts of known parent bodies. We review breccias in all types of asteroidal meteorites and focus on the formation of regolith breccias and the role of catastrophic impacts on asteroids. 1. GENERAL INTRODUCTION shock waves during collisional processes. Partsch (1843) and von Reichenbach (1860) described “polymict breccias” 1.1. -
Effects of Atmospheric Breakup on Crater Field Formation 1
ICARUS 42, 211--233 (1980) Effects of Atmospheric Breakup on Crater Field Formation 1 QUINN R. PASSEY AND H. J. MELOSH z Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125 Received October 5, 1979; revised February 18, 1980 This paper investigates the physics of meteoroid breakup in the atmosphere and its implications for the observed features of strewn fields. There are several effects which cause dispersion of the meteoroid fragments: gravity, differential lift of the fragments, bow shock interaction just after breakup, centripetal separation by a rotating meteroid, and possibly a dynamical transverse separation resulting from the crushing deceleration in the atmosphere. Of these, we show that gravity alone can produce the common pattern in which the largest crater occurs at the downrange end of the scatter ellipse. The average lift-to-drag ratio of the tumbling fragments must be less than about 10 -3, otherwise small fragments would produce small craters downrange of the main crater, and this is not generally observed. The cross-range dispersion is probably due to the combined effects of bow shock interaction, crushing deceleration, and possibly spinning of the meteoroid. A number of terrestrial strewn fields are discussed in the light of these ideas, which are formulated quantitatively for a range of meteoroid velocities, entry angles, and crushing strengths. It is found that when the crater size exceeds about 1 km, the separation between the fragments upon landing is a fraction of their own diameter, so that the crater formed by such a fragmented meteoroid is almost indistinguishable from that formed by a solid body of the same total mass and velocity. -
The Stubenberg Meteorite - an LL6 Chondrite Fragmental Breccia Recovered Soon After Precise Prediction of the Strewn Field
The Stubenberg meteorite - an LL6 chondrite fragmental breccia recovered soon after precise prediction of the strewn field Addi BISCHOFF1, Jean-Alix BARRAT2, Kerstin BAUER3, Christoph BURKHARDT1, Henner BUSEMANN3, Samuel EBERT1, Michael GONSIOR4, Janina HAKENMÜLLER5, Jakub HALODA6, Dennis HARRIES7, Dieter HEINLEIN8, Harald HIESINGER1, Rupert HOCHLEITNER9 , Viktor HOFFMANN10, Melanie KALIWODA9, Matthias LAUBENSTEIN11, Colin MADEN3, Matthias M. M. MEIER3, Andreas MORLOK1, Andreas PACK12, Alexander RUF13,14, Philippe SCHMITT-KOPPLIN13,14, Maria SCHÖNBÄCHLER3, Robert C. J. STEELE3, Pavel SPURNÝ15, and Karl WIMMER16 1Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm-Klemm Str. 10, D-48149 Münster, Germany. 2Université de Bretagne Occidentale, Institut Universitaire Européen de la Mer, Place Nicolas Copernic, F-29280 Plouzané Cedex, France. 3ETH Zurich, Departement Erdwissenschaften, Clausiusstraße 25, CH-8092 Zurich, Switzerland. 4University of Maryland, Center for Environmental Science, Chesapeake Biological Laboratory, 146 Williams Street, Solomons, MD-20688, USA. 5Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany. 6Czech Geological Survey, Geologická 6, CZ-152 00 Praha 5, Czech Republic. 7Friedrich-Schiller-Universität Jena, Institut für Geowissenschaften, Carl-Zeiss-Promenade 10, D-07745 Jena, Germany. 8German Fireball Network, Lilienstraße 3, D-86156 Augsburg, Germany. 9Mineralogische Staatssammlung München (SNSB), Theresienstr. 41, D-80333 München, Germany. 10Department of Geosciences, -
The Jurassic Meteorite Flux: a Record from Extraterrestrial Chrome-Spinels
THE JURASSIC METEORITE FLUX: A RECORD FROM EXTRATERRESTRIAL CHROME-SPINELS A DISSERTATION SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI‘I AT MĀNOA IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN EARTH & PLANETARY SCIENCE December 2020 By Caroline E. Caplan Dissertation Committee: Gary R. Huss, Chairperson Kazu Nagashima Hope A. Ishii Greg Ravizza Schelte J. Bus Keywords: chrome-spinel, chromite, Jurassic, meteorites, oxygen isotopes To my ten-year-old self who wanted this for so long, you did it! ii ACKNOWLEDGMENTS Graduate school will forever be one of my favorite times in life. Through its ups and downs I have become more knowledgeable, confident, and have found true joy in science. I am especially thankful to my advisor, Gary Huss, without whom none of this work would have been possible. He has guided me through graduate school to grow as researcher, including giving me the opportunities to explore new avenues of my work. I would also like to thank my committee members: Kazu Nagashima for always answering my questions with patience, Hope Ishii for work and life guidance, Greg Ravizza for his excitement and new perspectives, and Bobby Bus for help with statistics and his endless curiosity. Thanks to Birger Schmitz who allowed me to work on such a special project and for the incredible opportunity to travel to Sweden, Russia, and Italy to obtain a better understanding of my samples and the area of work. I would also like to thank the HIGP and ERTH (GG) departments for fostering a productive and friendly environment. -
Asteroid 2008 TC3—Almahata Sitta: a Spectacular Breccia Containing Many Different Ureilitic and Chondritic Lithologies
Meteoritics & Planetary Science 45, Nr 10–11, 1638–1656 (2010) doi: 10.1111/j.1945-5100.2010.01108.x Asteroid 2008 TC3—Almahata Sitta: A spectacular breccia containing many different ureilitic and chondritic lithologies Addi BISCHOFF1*, Marian HORSTMANN1, Andreas PACK2, Matthias LAUBENSTEIN3, and Siegfried HABERER4 1Institut fu¨ r Planetologie, Wilhelm-Klemm-Str. 10, 48149 Mu¨ nster, Germany 2Geowissenschaftliches Zentrum, Universita¨ tGo¨ ttingen, Goldschmidtstrasse 1, 37077 Go¨ ttingen, Germany 3Laboratori Nazionali del Gran Sasso—I.N.F.N., S.S.17 ⁄ bis, km 18+910, I-67010 Assergi (AQ), Italy 4Haberer-Meteorites, Ruhbankweg 15, 79111 Freiburg, Germany *Corresponding author. E-mail: [email protected] (Received 24 February 2010; revision accepted 11 August 2010) Abstract–Asteroid 2008 TC3 impacted Earth in northern Sudan on October 7, 2008. The meteorite named Almahata Sitta was classified as a polymict ureilite. In this study, 40 small pieces from different fragments collected in the Almahata Sitta strewn field were investigated and a large number of different lithologies were found. Some of these fragments are ureilitic in origin, whereas others are clearly chondritic. As all are relatively fresh (W0–W0 ⁄ 1) and as short-lived cosmogenic radioisotopes were detected within two of the chondritic fragments, there is strong evidence that most, if not all belong to the Almahata Sitta meteorite fall. The fragments can roughly be subdivided into achondritic (ureilitic; 23 samples) and chondritic lithologies (17 samples). Among the ureilitic rocks are at least 10 different lithologies. A similar number of different chondritic lithologies also exist. Most chondritic fragments belong to at least seven different E-chondrite rock types (EH3, EL3 ⁄ 4, EL6, EL breccias, several different types of EL and EH impact melt rocks and impact melt breccias; some of the latter are shock-darkened). -
Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery, and Characterization
Research Articles panchromatic luminous efficiency was 7 ± 3%. Theoretical estimates under Chelyabinsk Airburst, Damage these conditions range from 5.6−13.2% (10). Assessment, Meteorite Recovery, and Calibrated video observations pro- vided a trajectory and pre-atmospheric orbit (Table 1) (SM Sect. 1.1). The Characterization fireball was first recorded at 97 km 1 2,3 4 altitude, moving at 19.16 ± 0.15 km/s Olga P. Popova, Peter Jenniskens, * Vacheslav Emel’yanenko, and entry angle 18.3 ± 0.2° with respect Anna Kartashova,4 Eugeny Biryukov,5 Sergey Khaibrakhmanov,6 1 1 6 to the horizon, which is slightly faster Valery Shuvalov, Yurij Rybnov, Alexandr Dudorov, Victor I. than reported earlier (11). Combined Grokhovsky,7 Dmitry D. Badyukov,8 Qing-Zhu Yin,9 Peter S. Gural,2 2 10 11,12 11 with the best kinetic energy estimate, an Jim Albers, Mikael Granvik, Läslo G. Evers, Jacob Kuiper, entry mass of 1.3 × 107 kg (with a fac- Vladimir Kharlamov,1 Andrey Solovyov,13 Yuri S. Rusakov,14 15 16 8 tor of two uncertainty) and a diameter Stanislav Korotkiy, Ilya Serdyuk, Alexander V. Korochantsev, of 19.8 ± 4.6 m is derived, assuming a Michail Yu Larionov,7 Dmitry Glazachev,1 Alexander E. Mayer,6 17 18 9 spherical shape and the meteorite- Galen Gisler, Sergei V. Gladkovsky, Josh Wimpenny, Matthew 3 9 9 9 derived density of 3.3 g/cm based on E. Sanborn, Akane Yamakawa, Kenneth L. Verosub, Douglas J. x-ray computed tomography (SM Sect. Rowland,19 Sarah Roeske,9 Nicholas W. Botto,9 Jon M.