The Meteoritical Society Newsletter 2001
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Ernst Zinner, Lithic Astronomer
UCLA UCLA Previously Published Works Title Ernst Zinner, lithic astronomer Permalink https://escholarship.org/uc/item/0gq43750 Journal Meteoritics & Planetary Science, 42(7/8) ISSN 1086-9379 Author Mckeegan, Kevin D. Publication Date 2007-07-01 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Meteoritics & Planetary Science 42, Nr 7/8, 1045–1054 (2007) Abstract available online at http://meteoritics.org Ernst Zinner, lithic astronomer Kevin D. MCKEEGAN Department of Earth and Space Sciences, University of California, Los Angeles, Los Angeles, California 90095–1567, USA E-mail: [email protected] It is a rare privilege to be one of the founders of an entirely new field of science, and it is especially remarkable when that new field belongs to the oldest branch of “natural philosophy.” The nature of the stars has perplexed and fascinated humanity for millennia. While the sources of their luminosity and their structures and evolution were revealed over the last century, it is thanks to the pioneering efforts of a rare and remarkable man, Ernst Zinner, as well as his colleagues and students (mostly at the University of Chicago and at Washington University in Saint Louis), that in the last two decades it has become possible to literally hold a piece of a star in one’s hand. Armed with sophisticated microscopes and mass spectrometers of various sorts, these “lithic astronomers” are able to reveal stellar processes in exquisite detail by examining the chemical, mineralogical, and especially the nuclear properties of these microscopic grains of stardust. With this special issue of Meteoritics & Planetary Science, we honor Ernst Zinner (Fig. -
Meteorites and Impacts: Research, Cataloguing and Geoethics
Seminario_10_2013_d 10/6/13 17:12 Página 75 Meteorites and impacts: research, cataloguing and geoethics / Jesús Martínez-Frías Centro de Astrobiología, CSIC-INTA, asociado al NASA Astrobiology Institute, Ctra de Ajalvir, km. 4, 28850 Torrejón de Ardoz, Madrid, Spain Abstract Meteorites are basically fragments from asteroids, moons and planets which travel trough space and crash on earth surface or other planetary body. Meteorites and their impact events are two topics of research which are scientifically linked. Spain does not have a strong scientific tradition of the study of meteorites, unlike many other European countries. This contribution provides a synthetic overview about three crucial aspects related to this subject: research, cataloging and geoethics. At present, there are more than 20,000 meteorite falls, many of them collected after 1969. The Meteoritical Bulletin comprises 39 meteoritic records for Spain. The necessity of con- sidering appropriate protocols, scientific integrity issues and a code of good practice regarding the study of the abiotic world, also including meteorites, is emphasized. Resumen Los meteoritos son, básicamente, fragmentos procedentes de los asteroides, la Luna y Marte que chocan contra la superficie de la Tierra o de otro cuerpo planetario. Su estudio está ligado científicamente a la investigación de sus eventos de impacto. España no cuenta con una fuerte tradición científica sobre estos temas, al menos con el mismo nivel de desarrollo que otros paí- ses europeos. En esta contribución se realiza una revisión sintética de tres aspectos cruciales relacionados con los meteoritos: su investigación, catalogación y geoética. Hasta el momento se han reconocido más de 20.000 caídas meteoríticas, muchas de ellos desde 1969. -
Experimental and Petrological Constraints on Lunar Differentiation from the Apollo 15 Green Picritic Glasses
Meteoritics & Planetary Science 38, Nr 4, 515–527(2003) Abstract available online at http://meteoritics.org Experimental and petrological constraints on lunar differentiation from the Apollo 15 green picritic glasses Linda T. ELKINS-TANTON,1* Nilanjan CHATTERJEE,2 and Timothy L. GROVE2 1Department of Geological Sciences, Brown University, Providence, Rhode Island, 02912, USA 2Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA *Corresponding author: [email protected] (Received 15 July 2002; revision accepted 23 September 2002) Abstract–Phase equilibrium experiments on the most magnesian Apollo 15C green picritic glass composition indicate a multiple saturation point with olivine and orthopyroxene at 1520°C and 1.3 GPa (about 260 km depth in the moon). This composition has the highest Mg# of any lunar picritic glass and the shallowest multiple saturation point. Experiments on an Apollo 15A composition indicate a multiple saturation point with olivine and orthopyroxene at 1520°C and 2.2 GPa (about 440 km depth in the moon). The importance of the distinctive compositional trends of the Apollo 15 groups A, B, and C picritic glasses merits the reanalysis of NASA slide 15426,72 with modern electron microprobe techniques. We confirm the compositional trends reported by Delano (1979, 1986) in the major element oxides SiO2, TiO2, Al2O3, Cr2O3, FeO, MnO, MgO, and CaO, and we also obtained data for the trace elements P2O5, K2O, Na2O, NiO, S, Cu, Cl, Zn, and F. Petrogenetic modeling demonstrates that the Apollo 15 A-B-C glass trends could not have been formed by fractional crystallization or any continuous assimilation/fractional crystallization (AFC) process. -
OPENING CEREMONY 9:00 A.M
81st Annual Meeting of The Meteoritical Society 2018 (LPI Contrib. No. 2067) sess201.pdf Monday, July 23, 2018 OPENING CEREMONY 9:00 a.m. Concert Hall of the Academy of Science Building 9:00 a.m. Opening Ceremony Marina Ivanova, Vernadsky Institute, Convener for 81st Annual Meeting of The Meteoritical Society Eric Galimov, Vernadsky Institute, Scientific Advisor Dmitry Badyukov, Vernadsky Institute, Head of the Meteoritics Laboratory AWARD CEREMONY 9:30 a.m. Concert Hall of the Academy of Science Building Chairs: Trevor Ireland Meenakshi Wadhwa 9:30 a.m. Leonard Medal Recipient: Alexander N. Krot Citation: Kevin D. McKeegan The Leonard Medal is given to individuals who have made outstanding original contributions to the science of meteoritics or closely allied fields. The Meteoritical Society recognizes Alexander “Sasha” Krot with its 2018 Leonard Medal in recognition of his fundamental contributions to understanding the role oxygen isotopes in early solar system processes and aqueous alteration processes on asteroids. 9:45 a.m. Barringer Medal Recipient: Thomas Kenkmann Citation: Kai Wünnemann The Barringer Medal is given for outstanding work in the field of impact crating. The 2018 Barringer Medal is awarded to Professor Thomas Kenkmann for his fundamental contributions to our understanding of the structure mechanics and tectonics of rock displacement associated with the formation of hypervelocity impact craters. 10:00 a.m. Nier Prize Recipient: Lydia Hallis Citation: Martin Lee The Nier Prize is given for significant research in the field of meteoritics and closely related fields by a young scientist under the age of 35. The Meteoritical Society recognizes Lydia Hallis with its 2018 Nier Prize for her contributions to the understanding of the origin of volatiles in planets. -
Curriculum Vitae
DANTE S. LAURETTA Lunar and Planetary Laboratory Department of Planetary Sciences University of Arizona Tucson, AZ 85721-0092 Cell: (520) 609-2088 Email: [email protected] CHRONOLOGY OF EDUCATION Washington University, St. Louis, MO Dept. of Earth and Planetary Sciences Ph.D. in Earth and Planetary Sciences, 1997 Thesis: Theoretical and Experimental Studies of Fe-Ni-S, Be, and B Cosmochemistry Advisor: Bruce Fegley, Jr. University of Arizona, Tucson, AZ Depts. of Physics, Mathematics, and East Asian Studies B.S. in Physics and Mathematics, Cum Laude, 1993 B.A. in Oriental Studies (emphasis: Japanese), Cum Laude, 1993 CHRONOLOGY OF EMPLOYMENT Professor, Lunar and Planetary Laboratory, Dept. of Planetary Sciences, University of Arizona, Tucson, AZ; 2012 – present. Principal Investigator, OSIRIS-REx Asteroid Sample Return Mission, NASA New Frontiers Program, 2011 – present. Deputy Principal Investigator, OSIRIS-REx Asteroid Sample Return Mission, NASA New Frontiers Program, 2008 – 2011. Associate Professor, Lunar and Planetary Laboratory, Dept. of Planetary Sciences, University of Arizona, Tucson, AZ; 2006 – 2012. Assistant Professor, Lunar and Planetary Laboratory, Dept. of Planetary Sciences, University of Arizona, Tucson, AZ; 2001 – 2006. Associate Research Scientist, Dept. of Chemistry & Biochemistry, Arizona State University, Tempe, AZ; 1999 – 2001. Postdoctoral Research Associate, Dept. of Geology, Arizona State University, Tempe, AZ Primary project: Transmission electron microscopy of meteoritic minerals. Supervisor: Peter R. Buseck; Dates: 1997 – 1999. Research Assistant, Dept. of Earth and Planetary Sciences, Washington Univ., St. Louis, MO Primary project: Experimental studies of sulfide formation in the solar nebula. Advisor: Bruce Fegley, Jr.; Dates: 1993 – 1997. Research Intern, NASA Undergraduate Research Program, University of Arizona, Tucson, AZ Primary project: Development of a logic-based language for S.E.T.I. -
Origins of Life: Transition from Geochemistry to Biogeochemistry
December 2016 Volume 12, Number 6 ISSN 1811-5209 Origins of Life: Transition from Geochemistry to Biogeochemistry NITA SAHAI and HUSSEIN KADDOUR, Guest Editors Transition from Geochemistry to Biogeochemistry Staging Life: Warm Seltzer Ocean Incubating Life: Prebiotic Sources Foundation Stones to Life Prebiotic Metal-Organic Catalysts Protometabolism and Early Protocells pub_elements_oct16_1300&icpms_Mise en page 1 13-Sep-16 3:39 PM Page 1 Reproducibility High Resolution igh spatial H Resolution High mass The New Generation Ion Microprobe for Path-breaking Advances in Geoscience U-Pb dating in 91500 zircon, RF-plasma O- source Addressing the growing demand for small scale, high resolution, in situ isotopic measurements at high precision and productivity, CAMECA introduces the IMS 1300-HR³, successor of the internationally acclaimed IMS 1280-HR, and KLEORA which is derived from the IMS 1300-HR³ and is fully optimized for advanced U-Th-Pb mineral dating. • New high brightness RF-plasma ion source greatly improving spatial resolution, reproducibility and throughput • New automated sample loading system with motorized sample height adjustment, significantly increasing analysis precision, ease-of-use and productivity • New UV-light microscope for enhanced optical image resolution (developed by University of Wisconsin, USA) ... and more! Visit www.cameca.com or email [email protected] to request IMS 1300-HR³ and KLEORA product brochures. Laser-Ablation ICP-MS ~ now with CAMECA ~ The Attom ES provides speed and sensitivity optimized for the most demanding LA-ICP-MS applications. Corr. Pb 207-206 - U (238) Recent advances in laser ablation technology have improved signal 2SE error per sample - Pb (206) Combined samples 0.076121 +/- 0.002345 - Pb (207) to background ratios and washout times. -
Modelling Bennu's Crater Development
EPSC Abstracts Vol. 14, EPSC2020-442, 2020 https://doi.org/10.5194/epsc2020-442 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Modelling Bennu's Crater Development Peter Smith, Daniella DellaGiustina, Keara Burke, Dathon Golish, and Dante Lauretta University of Arizona, Planetary Sciences, Tucson, United States of America ([email protected]) Modeling Bennu’s Crater Development P.H. Smith (1), D.N. DellaGiustina (1), K.N. Burke (1), D.R. Golish (1), D. S. Lauretta (1) (1) Lunar and Planetary Laboratory, University of Arizona, USA ([email protected]) Introduction Several hundred craters have been identified and mapped on Bennu [1]. Their spectral properties have been studied using data from the MapCam instrument onboard the OSIRIS-REx spacecraft [2]. The crater frequency versus spectral slope across the wavelength range of 0.550 µm (v band) to 0.860 µm (x band) shows a skewed distribution varying from the median spectral slope of –0.17 micron–1 (x/v = 0.948) to a neutral or flat slope (x/v = 1.0). DellaGiustina et al. [2] attribute this trend to space weathering. They suggest that freshly formed craters are red, and as they age, they evolve to the bluish slope seen across the asteroidal surface. This abstract presents the results of an age model of Bennu’s craters in the size range of 1 to 10 m. Craters in this size range were selected as having likely been formed during the time that Bennu has orbited in near-Earth space. -
Chondrule Sizes, We Have Compiled and Provide Commentary on Available Chondrule Dimension Literature Data
Invited review Chondrule size and related physical properties: a compilation and evaluation of current data across all meteorite groups. Jon M. Friedricha,b,*, Michael K. Weisbergb,c,d, Denton S. Ebelb,d,e, Alison E. Biltzf, Bernadette M. Corbettf, Ivan V. Iotzovf, Wajiha S. Khanf, Matthew D. Wolmanf a Department of Chemistry, Fordham University, Bronx, NY 10458 USA b Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024 USA c Department of Physical Sciences, Kingsborough College of the City University of New York, Brooklyn, NY 11235, USA d Graduate Center of the City University of New York, 365 5th Ave, New York, NY 10016 USA e Lamont-Doherty Earth Observatory, Columbia University, Palisades, New York 10964 USA f Fordham College at Rose Hill, Fordham University, Bronx, NY 10458 USA In press in Chemie der Erde – Geochemistry 21 August 2014 *Corresponding Author. Tel: +718 817 4446; fax: +718 817 4432. E-mail address: [email protected] 2 ABSTRACT The examination of the physical properties of chondrules has generally received less emphasis than other properties of meteorites such as their mineralogy, petrology, and chemical and isotopic compositions. Among the various physical properties of chondrules, chondrule size is especially important for the classification of chondrites into chemical groups, since each chemical group possesses a distinct size-frequency distribution of chondrules. Knowledge of the physical properties of chondrules is also vital for the development of astrophysical models for chondrule formation, and for understanding how to utilize asteroidal resources in space exploration. To examine our current knowledge of chondrule sizes, we have compiled and provide commentary on available chondrule dimension literature data. -
Lifetimes of Interstellar Dust from Cosmic Ray Exposure Ages of Presolar Silicon Carbide
Lifetimes of interstellar dust from cosmic ray exposure ages of presolar silicon carbide Philipp R. Hecka,b,c,1, Jennika Greera,b,c, Levke Kööpa,b,c, Reto Trappitschd, Frank Gyngarde,f, Henner Busemanng, Colin Madeng, Janaína N. Ávilah, Andrew M. Davisa,b,c,i, and Rainer Wielerg aRobert A. Pritzker Center for Meteoritics and Polar Studies, The Field Museum of Natural History, Chicago, IL 60605; bChicago Center for Cosmochemistry, The University of Chicago, Chicago, IL 60637; cDepartment of the Geophysical Sciences, The University of Chicago, Chicago, IL 60637; dNuclear and Chemical Sciences Division, Lawrence Livermore National Laboratory, Livermore, CA 94550; ePhysics Department, Washington University, St. Louis, MO 63130; fCenter for NanoImaging, Harvard Medical School, Cambridge, MA 02139; gInstitute of Geochemistry and Petrology, ETH Zürich, 8092 Zürich, Switzerland; hResearch School of Earth Sciences, The Australian National University, Canberra, ACT 2601, Australia; and iEnrico Fermi Institute, The University of Chicago, Chicago, IL 60637 Edited by Mark H. Thiemens, University of California San Diego, La Jolla, CA, and approved December 17, 2019 (received for review March 15, 2019) We determined interstellar cosmic ray exposure ages of 40 large ago. These grains are identified as presolar by their large isotopic presolar silicon carbide grains extracted from the Murchison CM2 anomalies that exclude an origin in the Solar System (13, 14). meteorite. Our ages, based on cosmogenic Ne-21, range from 3.9 ± Presolar stardust grains are the oldest known solid samples 1.6 Ma to ∼3 ± 2 Ga before the start of the Solar System ∼4.6 Ga available for study in the laboratory, represent the small fraction ago. -
Leshin Web CV Short Feb14
Laurie A. Leshin, Ph.D. Professional Experience WORCESTER POLYTECHNIC INSTITUTE, STARTING JULY, 2014 President RENSSELAER POLYTECHNIC INSTITUTE, 2011-PRESENT Dean, School of Science and Professor, Department of Earth & Environmental Sciences NATIONAL AERONAUTICS AND SPACE ADMINISTRATION, 2005-2011 Deputy Associate Administrator, Exploration Systems Mission Directorate, NASA HQ, 2010-2011 Deputy Center Director for Science & Technology, NASA Goddard Space Flight Center, 2008-2009 Director of Sciences and Exploration Directorate, NASA Goddard Space Flight Center, 2005-2007 ARIZONA STATE UNIVERSITY, 1998-2005 Interim Director, School of Earth and Space Exploration, Arizona State University, 2005 The Dee and John Whiteman Dean’s Distinguished Professor, Department of Geological Sciences, 2001 – 2005; Assistant Professor, 1998 – 2001 Director, Center for Meteorite Studies, 2003 – 2005; Associate Director, 2000 – 2002 UNIVERSITY OF CALIFORNIA, LOS ANGELES, 1994-1998 W. W. Rubey Faculty Fellow, Department of Earth and Space Sciences, 1996 – 1998 University of California President's Postdoctoral Fellow, Dept. of Earth and Space Sci., 1994 – 1996 Education Ph.D. 1994 California Institute of Technology, Pasadena, CA, Geochemistry M. S. 1989 California Institute of Technology, Pasadena, CA, Geochemistry B. S. 1987 Arizona State University, Tempe, AZ, Chemistry, summa cum laude Selected Professional and Community Service Advisory Board, National Air & Space Museum (appointed by President Obama), 2013-present Advisory Board, US Merchant Marine Academy -
Programme, (2016) 4Th International Workshop on Highly Siderophile Element Geochemistry
See discussions, stats, and author profiles for this publication at: https://www.researchgate.net/publication/324759584 Per request - Programme, (2016) 4th International Workshop on Highly Siderophile Element Geochemistry Research · July 2016 CITATIONS 0 1 author: Amy Riches 72 PUBLICATIONS 384 CITATIONS SEE PROFILE Some of the authors of this publication are also working on these related projects: 4th International Workshop on Highly Siderophile Element Geochemistry View project All content following this page was uploaded by Amy Riches on 25 April 2018. The user has requested enhancement of the downloaded file. Durham Geochemistry Centre Thank you to our sponsors who have made this workshop possible: 1 Welcome The event organisers are delighted to welcome, to the 4th International Workshop on Highly Siderophile Element Geochemistry, scientists of all career levels from academic institutions and government organisations from all over the globe. Durham University’s Department of Earth Sciences and its Geochemistry Group are thrilled to have brought together a large and diverse set of experts in HSE sciences, and we look forward to hosting a very productive meeting. Overview This specialist workshop is a 4 day event timed to occur between the 2016 Annual Goldschmidt Conference and the 79th Annual Meeting of the Meteoritical Society. It builds on the legacy of three highly-successful preceding meetings, the last of which took place in Durham in 2006 (then Chair, Dr. Ambre Luguet). This event also complements the short course on highly siderophile and strongly chalcophile elements in high temperature geochemistry and cosmochemistry held 7 months prior and linked to RiMG volume #81. The 4th International Workshop on Highly Siderophile Element Geochemistry is of cross-disciplinary appeal in covering analytical advances, as well as low-temperature and high-temperature geo- and cosmochemistry topics pertaining to HSEs and allied elements. -
Discoveries of Mass Independent Isotope Effects in the Solar System: Past, Present and Future Mark H
Reviews in Mineralogy & Geochemistry Vol. 86 pp. 35–95, 2021 2 Copyright © Mineralogical Society of America Discoveries of Mass Independent Isotope Effects in the Solar System: Past, Present and Future Mark H. Thiemens Department of Chemistry and Biochemistry University of California San Diego La Jolla, California 92093 USA [email protected] Mang Lin State Key Laboratory of Isotope Geochemistry Guangzhou Institute of Geochemistry, Chinese Academy of Sciences Guangzhou, Guangdong 510640 China University of Chinese Academy of Sciences Beijing 100049 China [email protected] THE BEGINNING OF ISOTOPES Discovery and chemical physics The history of the discovery of stable isotopes and later, their influence of chemical and physical phenomena originates in the 19th century with discovery of radioactivity by Becquerel in 1896 (Becquerel 1896a–g). The discovery catalyzed a range of studies in physics to develop an understanding of the nucleus and the properties influencing its stability and instability that give rise to various decay modes and associated energies. Rutherford and Soddy (1903) later suggested that radioactive change from different types of decay are linked to chemical change. Soddy later found that this is a general phenomenon and radioactive decay of different energies and types are linked to the same element. Soddy (1913) in his paper on intra-atomic charge pinpointed the observations as requiring the observations of the simultaneous character of chemical change from the same position in the periodic chart with radiative emissions required it to be of the same element (same proton number) but differing atomic weight. This is only energetically accommodated by a change in neutrons and it was this paper that the name “isotope” emerges.