Cometary Micrometeorites and Input of Prebiotic Compounds
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Accretion of Water in Carbonaceous Chondrites: Current Evidence and Implications for the Delivery of Water to Early Earth
ACCRETION OF WATER IN CARBONACEOUS CHONDRITES: CURRENT EVIDENCE AND IMPLICATIONS FOR THE DELIVERY OF WATER TO EARLY EARTH Josep M. Trigo-Rodríguez1,2, Albert Rimola3, Safoura Tanbakouei1,3, Victoria Cabedo Soto1,3, and Martin Lee4 1 Institute of Space Sciences (CSIC), Campus UAB, Facultat de Ciències, Torre C5-parell-2ª, 08193 Bellaterra, Barcelona, Catalonia, Spain. E-mail: [email protected] 2 Institut d’Estudis Espacials de Catalunya (IEEC), Edif.. Nexus, c/Gran Capità, 2-4, 08034 Barcelona, Catalonia, Spain 3 Departament de Química, Universitat Autònoma de Barcelona, 08193 Bellaterra, Catalonia, Spain. E-mail: [email protected] 4 School of Geographical and Earth Sciences, University of Glasgow, Gregory Building, Lilybank Gardens, Glasgow G12 8QQ, UK. Manuscript Pages: 37 Tables: 2 Figures: 10 Keywords: comet; asteroid; meteoroid; meteorite; minor bodies; primitive; tensile strength Accepted in Space Science Reviews (SPAC-D-18-00036R3, Vol. Ices in the Solar System) DOI: 10.1007/s11214-019-0583-0 Abstract: Protoplanetary disks are dust-rich structures around young stars. The crystalline and amorphous materials contained within these disks are variably thermally processed and accreted to make bodies of a wide range of sizes and compositions, depending on the heliocentric distance of formation. The chondritic meteorites are fragments of relatively small and undifferentiated bodies, and the minerals that they contain carry chemical signatures providing information about the early environment available for planetesimal formation. A current hot topic of debate is the delivery of volatiles to terrestrial planets, understanding that they were built from planetesimals formed under far more reducing conditions than the primordial carbonaceous chondritic bodies. -
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. -
Chondrites and Chondrules Analogous to Sediments Dr
Chondrites and Chondrules Analogous to Sediments Dr. Richard K. Herd Curator, National Meteorite Collection, Geological Survey of Canada, Natural Resources Canada (Retired) 51st Annual Lunar and Planetary Science Conference Houston, Texas March 16-20, 2020 Introduction and Summary • Comparing chondrites and terrestrial conglomerates [1] continues • Meteorites are fragmental rocks, continually subjected to impacts and collisions, whatever their ultimate origin in space and time • Space outside Earth’s atmosphere may be considered a 4D debris field • Of the debris that reaches the surface of Earth and is available for study, > 80 % are chondrites • Chondrites and chondrules are generally considered the product of heating of dust in the early Solar System, and therefore effectively igneous in origin • Modelling these abundant and important space rocks as analogous to terrestrial detrital sediments, specifically conglomerates, is innovative, can help derive data on their true origins and history, and provide con text for ongoing analyses Chondrites and Chondrules • Chondrites are rocks made of rocks • They are composed of chondrules and chondrule-like objects from which they take their name • Chondrules are roughly spheroidal pebble-like rocks predominantly composed of olivine, pyroxene, feldspar, iron-nickel minerals, chromite, magnetite, sulphides etc. • They range from nanoscale to more than a centimetre, with some size variation by chondrite type. There are thousands/millions of them available for study • Hundreds of chondrules fill the area of a single 3.5 x 2.5 cm standard thin section What is Known ? • Adjacent chondrules may be millions of years different in age • They date from the time of earliest solar system objects (viz. -
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. -
Addibischoffite, Ca2al6al6o20, a New Calcium Aluminate Mineral from The
1 Revision 3 2 Addibischoffite, Ca2Al6Al6O20, a new calcium aluminate mineral from 3 the Acfer 214 CH carbonaceous chondrite: A new refractory phase from 4 the solar nebula 5 Chi Ma1,*, Alexander N. Krot2, Kazuhide Nagashima2 6 1Division of Geological and Planetary Sciences, California Institute of Technology, 7 Pasadena, California 91125, USA 8 2Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, 9 Honolulu, Hawai‘i 96822, USA 10 11 ABSTRACT 12 Addibischoffite (IMA 2015-006), Ca2Al6Al6O20, is a new calcium aluminate mineral 13 that occurs with hibonite, perovskite, kushiroite, Ti-kushiroite, spinel, melilite, 14 anorthite and FeNi-metal in the core of a Ca-Al-rich inclusion (CAI) in the Acfer 15 214 CH3 carbonaceous chondrite. The mean chemical composition of type 16 addibischoffite by electron probe microanalysis is (wt%) Al2O3 44.63, CaO 15.36, 17 SiO2 14.62, V2O3 10.64, MgO 9.13, Ti2O3 4.70, FeO 0.46, total 99.55, giving rise to 18 an empirical formula of 3+ 3+ 2+ 19 (Ca2.00)(Al2.55Mg1.73V 1.08Ti 0.50Ca0.09Fe 0.05)Σ6.01(Al4.14Si1.86)O20. The general 20 formula is Ca2(Al,Mg,V,Ti)6(Al,Si)6O20. The end-member formula is Ca2Al6Al6O20. 21 Addibischoffite has the P1 aenigmatite structure with a = 10.367 Å, b = 10.756 Å, c 22 = 8.895 Å, α = 106.0°, β = 96.0°, γ = 124.7°, V = 739.7 Å3, and Z = 2, as revealed by 23 electron back-scatter diffraction. The calculated density using the measured 24 composition is 3.41 g/cm3. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
I-Xe Analysis of Enstatite Meteorites and a Eucrite
Testing an integrated chronology: I-Xe analysis of enstatite meteorites and a eucrite Item Type Article; text Authors Busfield, A.; Turner, G.; Gilmour, J. D. Citation Busfield, A., Turner, G., & Gilmour, J. D. (2008). Testing an integrated chronology: IXe analysis of enstatite meteorites and a eucrite. Meteoritics & Planetary Science, 43(5), 883-897. DOI 10.1111/j.1945-5100.2008.tb01087.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 26/09/2021 21:32:45 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656429 Meteoritics & Planetary Science 43, Nr 5, 883–897 (2008) AUTHOR’S PROOF Abstract available online at http://meteoritics.org Testing an integrated chronology: I-Xe analysis of enstatite meteorites and a eucrite A. BUSFIELD, G. TURNER, and J. D. GILMOUR* School of Earth, Atmospheric and Environmental Science, University of Manchester, Oxford Road, Manchester M13 9PL, UK *Corresponding author. E-mail: [email protected] (Supplementary tables and figures are available online at http://meteoritics.org/online supplements.htm) (Received 06 October 2006; revision accepted 21 November 2007) Abstract–We have determined initial 129I/127I ratios for mineral concentrates of four enstatite meteorites and a eucrite. In the case of the enstatite meteorites the inferred ages are associated with the pyroxene-rich separates giving pyroxene closure ages relative to the Shallowater standard of Indarch (EH4, 0.04 ± 0.67 Ma), Khairpur (EL6, −4.22 ± 0.67 Ma), Khor Temiki (aubrite, −0.06 Ma), and Itqiy (enstatite achondrite, −2.6 ± 2.6 Ma), negative ages indicate closure after Shallowater. -
Space Resources Roundtable II : November 8-10, 2000, Golden, Colorado
SPACE RESOURCES RouNDTABLE II November 8-10, 2000 Colorado School of Mines Golden, Colorado LPI Contribution No. 1070 SPACE RESOURCES ROUNDTABLE II November 8-10, 2000 Golden, Colorado Sponsored by Colorado School of Mines Lunar and Planetary Institute National Aeronautics and Space Administration Steering Committee Joe Burris, WorldTradeNetwork.net David Criswell, University of Houston Michael B. Duke, Lunar and Planetary Institute Mike O'Neal, NASA Kennedy Space Center Sanders Rosenberg, InSpace Propulsion, Inc. Kevin Reed, Marconi, Inc. Jerry Sanders, NASA Johnson Space Center Frank Schowengerdt, Colorado School of Mines Bill Sharp, Colorado School of Mines LPI Contribution No. 1070 Compiled in 2000 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. Matenal in this volume may be copied wnhout restraint for library, abstract service, education. or personal research purposes; however, republication of any paper or portion thereof requ1res the wriuen permission of the authors as well as the appropnate acknowledgment of this publication. Abstracts in this volume may be cited as Author A B. (2000) Title of abstract. In Space Resources Roundtable II. p x.x . LPI Contnbuuon No. 1070. Lunar and Planetary Institute. Houston. This repon is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Phone: 281-486-2172 Fax: 281-486-2186 E-mail: [email protected] Mail order requestors will be invoiced for the cost of shipping and handling. LPI Contribution No 1070 iii Preface This volume contains abstracts that have been accepted for presentation at the Space Resources Roundtable II, November 8-10, 2000. -
High Survivability of Micrometeorites on Mars: Sites with Enhanced Availability of Limiting Nutrients
RESEARCH ARTICLE High Survivability of Micrometeorites on Mars: Sites With 10.1029/2019JE006005 Enhanced Availability of Limiting Nutrients Key Points: Andrew G. Tomkins1 , Matthew J. Genge2,3 , Alastair W. Tait1,4 , Sarah L. Alkemade1, • Micrometeorites are predicted to be 1 1 5 far more abundant on Mars than on Andrew D. Langendam , Prudence P. Perry , and Siobhan A. Wilson Earth 1 2 • Micrometeorites are concentrated in School of Earth, Atmosphere and Environment, Melbourne, Victoria, Australia, Impact and Astromaterials Research the residue of aeolian sediment Centre, Department of Earth Science and Engineering, Imperial College London, London, UK, 3Department of removal, such as at bedrock cracks Mineralogy, The Natural History Museum, London, UK, 4Department of Biological and Environmental Sciences, and gravel accumulations University of Stirling, Scotland, UK, 5Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, • Micrometeorite accumulation sites are enriched in key nutrients for Alberta, Canada primitive microbes: reduced phosphorus, sulfur, and iron Abstract NASA's strategy in exploring Mars has been to follow the water, because water is essential for life, and it has been found that there are many locations where there was once liquid water on the surface. Now perhaps, to narrow down the search for life on a barren basalt‐dominated surface, there needs to be a Correspondence to: A. G. Tomkins, refocusing to a strategy of “follow the nutrients.” Here we model the entry of metallic micrometeoroids [email protected] through the Martian atmosphere, and investigate variations in micrometeorite abundance at an analogue site on the Nullarbor Plain in Australia, to determine where the common limiting nutrients available in Citation: these (e.g., P, S, Fe) become concentrated on the surface of Mars. -
Petrography and Mineral Chemistry of the Anhydrous Component of the Tagish Lake Carbonaceous Chondrite
Meteoritics & Planetary Science 38, Nr 5, 813–825 (2003) Abstract available online at http://meteoritics.org Petrography and mineral chemistry of the anhydrous component of the Tagish Lake carbonaceous chondrite S. B. SIMON1* and L. GROSSMAN1, 2 1Department of the Geophysical Sciences, 5734 South Ellis Avenue, The University of Chicago, Chicago, Illinois 60637, USA 2The Enrico Fermi Institute, 5640 South Ellis Avenue, The University of Chicago, Chicago, Illinois 60637, USA *Corresponding author. E-mail: [email protected] (Received 30 August 2002; revision accepted 16 January 2003) Abstract–Most studies of Tagish Lake have considered features that were either strongly affected by or formed during the extensive hydrous alteration experienced by this meteorite. This has led to some ambiguity as to whether Tagish Lake should be classified a CI, a CM, or something else. Unlike previous workers, we have focused upon the primary, anhydrous component of Tagish Lake, recovered through freeze-thaw disaggregation and density separation and located by thin section mapping. We found many features in common with CMs that are not observed in CIs. In addition to the presence of chondrules and refractory forsterite (which distinguish Tagish Lake from the CIs), we found hibonite-bearing refractory inclusions, spinel-rich inclusions, forsterite aggregates, Cr-, Al-rich spinel, and accretionary mantles on many clasts, which clearly establishes a strong link between Tagish Lake and the CM chondrites. The compositions of isolated olivine crystals in Tagish Lake are also like those found in CMs. We conclude that the anhydrous inclusion population of Tagish Lake was, originally, very much like that of the known CM chondrites and that the inclusions in Tagish Lake are heavily altered, more so than even those in Mighei, which are more heavily altered than those in Murchison. -
Connection Between Micrometeorites and Wild 2 Particles: from Antarctic Snow to Cometary Ices
Meteoritics & Planetary Science 44, Nr 10, 1643–1661 (2009) Abstract available online at http://meteoritics.org Connection between micrometeorites and Wild 2 particles: From Antarctic snow to cometary ices E. DOBRIC√1,*, C. ENGRAND1, J. DUPRAT1, M. GOUNELLE2, H. LEROUX3, E. QUIRICO4, and J.-N. ROUZAUD5 1Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse, CNRS-Univ. Paris Sud, 91405 Orsay Campus, France 2Laboratoire de Minéralogie et de Cosmochimie, Muséum National d’Histoire Naturelle, 57 rue Cuvier, CP52, 75005 Paris, France 3Laboratoire de Structure et Propriétés de l’Etat Solide, CNRS-Univ. des Sciences et Technologies de Lille, 59655 Villeneuve d’Ascq, France 4Laboratoire de Planétologie de Grenoble, Univ. J. Fourier CNRS-INSU 38041 Grenoble Cedex 09, France 5Laboratoire de Géologie, Ecole Normale Supérieure, CNRS, 75231 Paris Cedex 5, France *Corresponding author. E-mail: [email protected] (Received 17 March 2009; revision accepted 21 September 2009) Abstract–We discuss the relationship between large cosmic dust that represents the main source of extraterrestrial matter presently accreted by the Earth and samples from comet 81P/Wild 2 returned by the Stardust mission in January 2006. Prior examinations of the Stardust samples have shown that Wild 2 cometary dust particles contain a large diversity of components, formed at various heliocentric distances. These analyses suggest large-scale radial mixing mechanism(s) in the early solar nebula and the existence of a continuum between primitive asteroidal and cometary matter. The recent collection of CONCORDIA Antarctic micrometeorites recovered from ultra-clean snow close to Dome C provides the most unbiased collection of large cosmic dust available for analyses in the laboratory.