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Olivine and Pyroxene from the Mantle of Asteroid 4 Vesta ∗ Nicole G
Earth and Planetary Science Letters 418 (2015) 126–135 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Olivine and pyroxene from the mantle of asteroid 4 Vesta ∗ Nicole G. Lunning a, , Harry Y. McSween Jr. a,1, Travis J. Tenner b,2, Noriko T. Kita b,3, Robert J. Bodnar c,4 a Department of Earth and Planetary Sciences and Planetary Geosciences Institute, University of Tennessee, Knoxville, TN 37996, USA b Department of Geosciences, University of Wisconsin, Madison, WI 53706, USA c Department of Geosciences, Virginia Tech, Blacksburg, VA 24061, USA a r t i c l e i n f o a b s t r a c t Article history: A number of meteorites contain evidence that rocky bodies formed and differentiated early in our solar Received 25 September 2014 system’s history, and similar bodies likely contributed material to form the planets. These differentiated Received in revised form 25 February 2015 rocky bodies are expected to have mantles dominated by Mg-rich olivine, but direct evidence for such Accepted 25 February 2015 mantles beyond our own planet has been elusive. Here, we identify olivine fragments (Mg# = 80–92) in Available online 17 March 2015 howardite meteorites. These Mg-rich olivine fragments do not correspond to an established lithology Editor: T. Mather in the howardite–eucrite–diogenite (HED) meteorites, which are thought to be from the asteroid 4 Keywords: Vesta; their occurrence in howardite breccias, combined with diagnostic oxygen three-isotope signatures planetary formation and minor element chemistry, indicates they are vestan. -
Assessment of the Mesosiderite-Diogenite Connection and an Impact Model for the Genesis of Mesosiderites
45th Lunar and Planetary Science Conference (2014) 2554.pdf ASSESSMENT OF THE MESOSIDERITE-DIOGENITE CONNECTION AND AN IMPACT MODEL FOR THE GENESIS OF MESOSIDERITES. T. E. Bunch1,3, A. J. Irving2,3, P. H. Schultz4, J. H. Wittke1, S. M. Ku- ehner2, J. I. Goldstein5 and P. P. Sipiera3,6 1Dept. of Geology, SESES, Northern Arizona University, Flagstaff, AZ 86011 ([email protected]), 2Dept. of Earth & Space Sciences, University of Washington, Seattle, WA, 3Planetary Studies Foundation, Galena, IL, 4Dept. of Geological Sciences, Brown University, Providence, RI, 5Dept. of Geolo- gy, University of Massachusetts, Amherts, MA, 6Field Museum of Natural History, Chicago, IL. Introduction: Among well-recognized meteorite 34) is the most abundant silicate mineral and in some classes, the mesosiderites are perhaps the most com- clasts contains inclusions of FeS, tetrataenite, merrillite plex and petrogenetically least understood. Previous and silica. Three of the ten norite clasts contain a few workers have contributed important information about tiny grains of olivine (Fa24-32). A single, fine-grained “classic” falls and Antarctic finds, and have proposed breccia clast was found in NWA 5312 (see Figure 2). several different models for mesosiderite genesis [1]. Unlike the case of pallasites, the co-occurrence of met- al and silicates (predominantly orthopyroxene and cal- cic plagioclase) in mesosiderites is inconsistent with a single-stage “igneous” history, and instead seems to demand admixture of at least two separate compo- nents. Here we review the models in light of detailed ex- amination of multiple specimens from a very large mesosiderite strewnfield in Northwest Africa. Many specimens (totaling at least 80 kilograms) from this area (probably in Algeria) have been classified sepa- rately by us and others; however, in most cases the Figure 1. -
Physical Properties of Martian Meteorites: Porosity and Density Measurements
Meteoritics & Planetary Science 42, Nr 12, 2043–2054 (2007) Abstract available online at http://meteoritics.org Physical properties of Martian meteorites: Porosity and density measurements Ian M. COULSON1, 2*, Martin BEECH3, and Wenshuang NIE3 1Solid Earth Studies Laboratory (SESL), Department of Geology, University of Regina, Regina, Saskatchewan S4S 0A2, Canada 2Institut für Geowissenschaften, Universität Tübingen, 72074 Tübingen, Germany 3Campion College, University of Regina, Regina, Saskatchewan S4S 0A2, Canada *Corresponding author. E-mail: [email protected] (Received 11 September 2006; revision accepted 06 June 2007) Abstract–Martian meteorites are fragments of the Martian crust. These samples represent igneous rocks, much like basalt. As such, many laboratory techniques designed for the study of Earth materials have been applied to these meteorites. Despite numerous studies of Martian meteorites, little data exists on their basic structural characteristics, such as porosity or density, information that is important in interpreting their origin, shock modification, and cosmic ray exposure history. Analysis of these meteorites provides both insight into the various lithologies present as well as the impact history of the planet’s surface. We present new data relating to the physical characteristics of twelve Martian meteorites. Porosity was determined via a combination of scanning electron microscope (SEM) imagery/image analysis and helium pycnometry, coupled with a modified Archimedean method for bulk density measurements. Our results show a range in porosity and density values and that porosity tends to increase toward the edge of the sample. Preliminary interpretation of the data demonstrates good agreement between porosity measured at 100× and 300× magnification for the shergottite group, while others exhibit more variability. -
Evidence from Polymict Ureilite Meteorites for a Disrupted and Re-Accreted Single Ureilite Parent Asteroid Gardened by Several Distinct Impactors
Available online at www.sciencedirect.com Geochimica et Cosmochimica Acta 72 (2008) 4825–4844 www.elsevier.com/locate/gca Evidence from polymict ureilite meteorites for a disrupted and re-accreted single ureilite parent asteroid gardened by several distinct impactors Hilary Downes a,b,*, David W. Mittlefehldt c, Noriko T. Kita d, John W. Valley d a School of Earth Sciences, Birkbeck University of London, Malet Street, London WC1E 7HX, UK b Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX 77058, USA c Mail Code KR, NASA/Johnson Space Center, Houston, TX 77058, USA d Department of Geology and Geophysics, University of Wisconsin-Madison, 1215 W. Dayton St., Madison, WI 53706, USA Received 25 July 2007; accepted in revised form 24 June 2008; available online 17 July 2008 Abstract Ureilites are ultramafic achondrites that exhibit heterogeneity in mg# and oxygen isotope ratios between different meteor- ites. Polymict ureilites represent near-surface material of the ureilite parent asteroid(s). Electron microprobe analyses of >500 olivine and pyroxene clasts in several polymict ureilites reveal a statistically identical range of compositions to that shown by unbrecciated ureilites, suggesting derivation from a single parent asteroid. Many ureilitic clasts have identical compositions to the anomalously high Mn/Mg olivines and pyroxenes from the Hughes 009 unbrecciated ureilite (here termed the ‘‘Hughes cluster”). Some polymict samples also contain lithic clasts derived from oxidized impactors. The presence of several common distinctive lithologies within polymict ureilites is additional evidence that ureilites were derived from a single parent asteroid. In situ oxygen three isotope analyses were made on individual ureilite minerals and lithic clasts, using a secondary ion mass spectrometer (SIMS) with precision typically better than 0.2–0.4& (2SD) for d18O and d17O. -
Meteorite Dunite Breccia Mil 03443: a Probable Crustal Cumulate Closely Related to Diogenites from the Hed Parent Asteroid
METEORITE DUNITE BRECCIA MIL 03443: A PROBABLE CRUSTAL CUMULATE CLOSELY RELATED TO DIOGENITES FROM THE HED PARENT ASTEROID. David W Mittlefehldt, Astromateri- als Research Office, NASA/Johnson Space Center, Houston, Texas, USA, ([email protected]). Introduction: There are numerous types of differ- Metal is very rare, and occurs as grains a few microns entiated meteorites, but most represent either the crusts in size associated with troilite. or cores of their parent asteroids. Ureilites, olivine- pyroxene-graphite rocks, are exceptions; they are man- tle restites [1]. Dunite is expected to be a common mantle lithology in differentiated asteroids. In particu- lar, models of the eucrite parent asteroid contain large volumes of dunite mantle [2-4]. Yet dunites are very rare among meteorites, and none are known associated with the howardite, eucrite, diogenite (HED) suite. Spectroscopic measurements of 4 Vesta, the probable HED parent asteroid, show one region with an olivine signature [5] although the surface is dominated by ba- saltic and orthopyroxenitic material equated with eucrites and diogenites [6]. One might expect that a small number of dunitic or olivine-rich meteorites might be delivered along with the HED suite. The 46 gram meteoritic dunite MIL 03443 (Fig. 1) Figure 2. BSE image of MIL 03443 showing its gen- was recovered from the Miller Range ice field of Ant- eral fragmental breccia texture, and primary texture arctica. This meteorite was tentatively classified as a between olivine, orthopyroxene and chromite. mesosiderite because large, dunitic clasts are found in this type of meteorite, but it was noted that MIL 03443 could represent a dunite sample of the HED suite [7]. -
Olivine-Dominated Asteroids and Meteorites: Distinguishing Nebular and Igneous Histories
Meteoritics & Planetary Science 42, Nr 2, 155–170 (2007) Abstract available online at http://meteoritics.org Olivine-dominated asteroids and meteorites: Distinguishing nebular and igneous histories Jessica M. SUNSHINE1*, Schelte J. BUS2, Catherine M. CORRIGAN3, Timothy J. MCCOY4, and Thomas H. BURBINE5 1Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA 2University of Hawai‘i, Institute for Astronomy, Hilo, Hawai‘i 96720, USA 3Johns Hopkins University, Applied Physics Laboratory, Laurel, Maryland 20723–6099, USA 4Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, D.C. 20560–0119, USA 5Department of Astronomy, Mount Holyoke College, South Hadley, Massachusetts 01075, USA *Corresponding author. E-mail: [email protected] (Received 14 February 2006; revision accepted 19 November 2006) Abstract–Melting models indicate that the composition and abundance of olivine systematically co-vary and are therefore excellent petrologic indicators. However, heliocentric distance, and thus surface temperature, has a significant effect on the spectra of olivine-rich asteroids. We show that composition and temperature complexly interact spectrally, and must be simultaneously taken into account in order to infer olivine composition accurately. We find that most (7/9) of the olivine- dominated asteroids are magnesian and thus likely sampled mantles differentiated from ordinary chondrite sources (e.g., pallasites). However, two other olivine-rich asteroids (289 Nenetta and 246 Asporina) are found to be more ferroan. Melting models show that partial melting cannot produce olivine-rich residues that are more ferroan than the chondrite precursor from which they formed. Thus, even moderately ferroan olivine must have non-ordinary chondrite origins, and therefore likely originate from oxidized R chondrites or melts thereof, which reflect variations in nebular composition within the asteroid belt. -
JEM-EUSO: Meteor and Nuclearite Observations
Exp Astron DOI 10.1007/s10686-014-9375-4 ORIGINAL ARTICLE JEM-EUSO: Meteor and nuclearite observations M. Bertaina A. Cellino F. Ronga The JEM-EUSO· Collaboration· · Received: 22 August 2013 / Accepted: 24 February 2014 ©SpringerScience+BusinessMediaDordrecht2014 Abstract Meteor and fireball observations are key to the derivation of both the inven- tory and physical characterization of small solar system bodies orbiting in the vicinity of the Earth. For several decades, observation of these phenomena has only been possible via ground-based instruments. The proposed JEM-EUSO mission has the potential to become the first operational space-based platform to share this capabil- ity. In comparison to the observation of extremely energetic cosmic ray events, which is the primary objective of JEM-EUSO, meteor phenomena are very slow, since their typical speeds are of the order of a few tens of km/sec (whereas cosmic rays travel at light speed). The observing strategy developed to detect meteors may also be applied to the detection of nuclearites, which have higher velocities, a wider range of possible trajectories, but move well below the speed of light and can therefore be considered as slow events for JEM-EUSO. The possible detection of nuclearites greatly enhances the scientific rationale behind the JEM-EUSO mission. Keywords Meteors Nuclearites JEM-EUSO Space detectors · · · M. Bertaina (!) Dipartimento di Fisica, Universit`adiTorino,INFNTorino,viaP.Giuria1,10125Torino,Italy e-mail: [email protected] A. Cellino (!) INAF-Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese (TO), Italy e-mail: [email protected] F. Ronga (!) Istituto Nazionale di Fisica Nucleare - Laboratori Nazionali di Frascati, Via E. -
Howardite-Eucrite-Diogenite) Title PARENT BODY -PARTIAL MELT EXPERIMENTS on DIFFERENTIATION PROCESSES-( Dissertation 全文 )
EVOLUTION OF THE HED (Howardite-Eucrite-Diogenite) Title PARENT BODY -PARTIAL MELT EXPERIMENTS ON DIFFERENTIATION PROCESSES-( Dissertation_全文 ) Author(s) Isobe, Hiroshi Citation Kyoto University (京都大学) Issue Date 1991-03-23 URL http://dx.doi.org/10.11501/3053044 Right Type Thesis or Dissertation Textversion author Kyoto University 学位 申請論文 磯部博志 EVOLUTION OF THE HED (howardite-eucrite-diogenite) PARENT BODY -PARTIAL MELT EXPERIMENTS ON DIFFERENTIATION PROCESSES- Hiroshi ISOBE Department of Environmental Safety Research Japan Atomic Energy Research Institute Tokai, Ibaraki, 319-11, JAPAN CONTENTS Abstract 1 Introduction1 2 Experiments —starting materials and procedures13 2-1 Composition of the starting materials13 2-2 Experimental procedures19 3 Results and interpretation25 3-1 Mineral assemblages of the run products25 3-2 Composition of the melts and minerals34 4 Discussion60 4-1 Melting relations on the 'pseudo-liquidus' diagrams 60 4-2 Fractionation sequence71 4-3 Physical conditions of the solid-liquid separations 78 4-4 Summary of the present evolution model of HEDP-PB96 Acknowledgments98 References99 Appendix 1 Chemistry of HED and pallasite meteorites106 Appendix 2 Tables of compositions of run products116 Abstract Three series of melting experiments with a chondritic material, a eucrite-diogenite mixture, and a eucritic material were carried out using a one atmosphere gas mixing furnace to illustrate liquidus phase relation and chemical compositions of the phases. Locations of an olivine control line, olivine-pyroxene phase boundary -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
Brachinite-Paper.Pdf
Open Research Online The Open University’s repository of research publications and other research outputs Petrological, petrofabric, and oxygen isotopic study of five ungrouped meteorites related to brachinites Journal Item How to cite: Hasegawa, Hikari; Mikouchi, Takashi; Yamaguchi, Akira; Yasutake, Masahiro; Greenwood, Richard and Franchi, Ian A. (2019). Petrological, petrofabric, and oxygen isotopic study of five ungrouped meteorites related to brachinites. Meteoritics & Planetary Science, 54(4) pp. 752–767. For guidance on citations see FAQs. c 2019 The Meteoritical Society https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Proof Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1111/maps.13249 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk M A P S 13249-3018 Dispatch: 30.1.19 CE: Malarvizhi Journal Code Manuscript No. No. of pages: 16 PE: Nishanthan P. Meteoritics & Planetary Science 1–16 (2019) 1 doi: 10.1111/maps.13249 2 3 4 5 Petrological, petrofabric, and oxygen isotopic study of five ungrouped meteorites 6 related to brachinites 7 8 9 Hikari HASEGAWA 1*, Takashi MIKOUCHI1,2, Akira YAMAGUCHI 3,4, 10 1 Masahiro YASUTAKE5, Richard C. GREENWOOD6, and Ian A. FRANCHI6 11 12 1Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 13 113-0033, -
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. -
Apollo 17 Index
Preparation, Scanning, Editing, and Conversion to Adobe Portable Document Format (PDF) by: Ronald A. Wells University of California Berkeley, CA 94720 May 2000 A P O L L O 1 7 I N D E X 7 0 m m, 3 5 m m, A N D 1 6 m m P H O T O G R A P H S M a p p i n g S c i e n c e s B r a n c h N a t i o n a l A e r o n a u t i c s a n d S p a c e A d m i n i s t r a t i o n J o h n s o n S p a c e C e n t e r H o u s t o n, T e x a s APPROVED: Michael C . McEwen Lunar Screening and Indexing Group May 1974 PREFACE Indexing of Apollo 17 photographs was performed at the Defense Mapping Agency Aerospace Center under the direction of Charles Miller, NASA Program Manager, Aerospace Charting Branch. Editing was performed by Lockheed Electronics Company, Houston Aerospace Division, Image Analysis and Cartography Section, under the direction of F. W. Solomon, Chief. iii APOLLO 17 INDEX 70 mm, 35 mm, AND 16 mm PHOTOGRAPHS TABLE OF CONTENTS Page INTRODUCTION ................................................................................................................... 1 SOURCES OF INFORMATION .......................................................................................... 13 INDEX OF 16 mm FILM STRIPS ........................................................................................ 15 INDEX OF 70 mm AND 35 mm PHOTOGRAPHS Listed by NASA Photograph Number Magazine J, AS17–133–20193 to 20375.........................................