Do Comets Have Chondrules and Cais? Evidence from the Leonid Meteors
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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. -
1 Characterization of Cometary Activity of 67P/Churyumov-Gerasimenko
Characterization of cometary activity of 67P/Churyumov-Gerasimenko comet Abstract After 2.5 years from the end of the mission, the data provided by the ESA/Rosetta mission still leads to important results about 67P/Churyumov-Gerasimenko (hereafter 67P), belonging to the Jupiter Family Comets. Since comets are among the most primitive bodies of the Solar System, the understanding of their formation and evolution gives important clues about the early stages of our planetary system, including the scenarios of water delivery to Earth. At the present state of knowledge, 67P’s activity has been characterized by measuring the physical properties of the gas and dust coma, by detecting water ice patches on the nucleus surface and by analyzing some peculiar events, such as outbursts. We propose an ISSI International Team to build a more complete scenario of the 67P activity during different stages of its orbit. The retrieved results in terms of dust emission, morphology and composition will be linked together in order to offer new insights about 67P formation and evolution. In particular the main goals of the project are: 1. Retrieval of the activity degree of different 67P geomorphological nucleus regions in different time periods, by reconstructing the motion of the dust particles revealed in the coma; 2. Identification of the main drivers of cometary activity, by studying the link between cometary activity and illumination/local time, dust morphology, surface geomorphology, dust composition. The project will shed light on how (and if) cometary activity is related to surface geology and/or composition or is just driven by local illumination. -
Stardust Comet Flyby
NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Stardust Comet Flyby Press Kit January 2004 Contacts Don Savage Policy/Program Management 202/358-1727 NASA Headquarters, Washington DC Agle Stardust Mission 818/393-9011 Jet Propulsion Laboratory, Pasadena, Calif. Vince Stricherz Science Investigation 206/543-2580 University of Washington, Seattle, WA Contents General Release ……………………………………......………….......................…...…… 3 Media Services Information ……………………….................…………….................……. 5 Quick Facts …………………………………………..................………....…........…....….. 6 Why Stardust?..................…………………………..................………….....………......... 7 Other Comet Missions ....................................................................................... 10 NASA's Discovery Program ............................................................................... 12 Mission Overview …………………………………….................……….....……........…… 15 Spacecraft ………………………………………………..................…..……........……… 25 Science Objectives …………………………………..................……………...…........….. 34 Program/Project Management …………………………...................…..…..………...... 37 1 2 GENERAL RELEASE: NASA COMET HUNTER CLOSING ON QUARRY Having trekked 3.2 billion kilometers (2 billion miles) across cold, radiation-charged and interstellar-dust-swept space in just under five years, NASA's Stardust spacecraft is closing in on the main target of its mission -- a comet flyby. "As the saying goes, 'We are good to go,'" said project manager Tom Duxbury at NASA's Jet -
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. -
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. -
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. -
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. -
Dust-To-Gas and Refractory-To-Ice Mass Ratios of Comet 67P
Dust-to-Gas and Refractory-to-Ice Mass Ratios of Comet 67P/Churyumov-Gerasimenko from Rosetta Observations Mathieu Choukroun, Kathrin Altwegg, Ekkehard Kührt, Nicolas Biver, Dominique Bockelée-Morvan, Joanna Drążkowska, Alain Hérique, Martin Hilchenbach, Raphael Marschall, Martin Pätzold, et al. To cite this version: Mathieu Choukroun, Kathrin Altwegg, Ekkehard Kührt, Nicolas Biver, Dominique Bockelée-Morvan, et al.. Dust-to-Gas and Refractory-to-Ice Mass Ratios of Comet 67P/Churyumov-Gerasimenko from Rosetta Observations. Journal Space Science Reviews, 2020, 10.1007/s11214-020-00662-1. hal- 03021621 HAL Id: hal-03021621 https://hal.archives-ouvertes.fr/hal-03021621 Submitted on 29 Aug 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Distributed under a Creative Commons Attribution| 4.0 International License Space Sci Rev (2020) 216:44 https://doi.org/10.1007/s11214-020-00662-1 Dust-to-Gas and Refractory-to-Ice Mass Ratios of Comet 67P/Churyumov-Gerasimenko from Rosetta Observations Mathieu Choukroun1 · Kathrin Altwegg2 · Ekkehard Kührt3 · Nicolas Biver4 · Dominique Bockelée-Morvan4 · Joanna Dra˙ ˛zkowska5 · Alain Hérique6 · Martin Hilchenbach7 · Raphael Marschall8 · Martin Pätzold9 · Matthew G.G.T. Taylor10 · Nicolas Thomas2 Received: 17 May 2019 / Accepted: 19 March 2020 / Published online: 8 April 2020 © The Author(s) 2020 Abstract This chapter reviews the estimates of the dust-to-gas and refractory-to-ice mass ratios derived from Rosetta measurements in the lost materials and the nucleus of 67P/Churyumov-Gerasimenko, respectively. -
The Thermal Conductivity of Meteorites: New Measurements and Analysis
This article appeared in a journal published by Elsevier. The attached copy is furnished to the author for internal non-commercial research and education use, including for instruction at the authors institution and sharing with colleagues. Other uses, including reproduction and distribution, or selling or licensing copies, or posting to personal, institutional or third party websites are prohibited. In most cases authors are permitted to post their version of the article (e.g. in Word or Tex form) to their personal website or institutional repository. Authors requiring further information regarding Elsevier’s archiving and manuscript policies are encouraged to visit: http://www.elsevier.com/copyright Author's personal copy Icarus 208 (2010) 449–454 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The thermal conductivity of meteorites: New measurements and analysis C.P. Opeil a, G.J. Consolmagno b,*, D.T. Britt c a Department of Physics, Boston College, Chestnut Hill, MA 02467-3804, USA b Specola Vaticana, V-00120, Vatican City State c Department of Physics, University of Central Florida, Orlando, FL 32816-2385, USA article info abstract Article history: We have measured the thermal conductivity at low temperatures (5–300 K) of six meteorites represent- Received 6 October 2009 ing a range of compositions, including the ordinary chondrites Cronstad (H5) and Lumpkin (L6), the Revised 21 January 2010 enstatite chondrite Abee (E4), the carbonaceous chondrites NWA 5515 (CK4 find) and Cold Bokkeveld Accepted 23 January 2010 (CM2), and the iron meteorite Campo del Cielo (IAB find). All measurements were made using a Quantum Available online 1 February 2010 Design Physical Properties Measurement System, Thermal Transport Option (TTO) on samples cut into regular parallelepipeds of 2–6 mm dimension.