Daniel T. Britt
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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. -
TUPELO, a NEW EL6 ENSTATITE CHONDRITE. DR Dunlap1
44th Lunar and Planetary Science Conference (2013) 2088.pdf TUPELO, A NEW EL6 ENSTATITE CHONDRITE. D. R. Dunlap1 ([email protected]), M. L. Pewitt1 ([email protected]), H. Y. McSween1, Raymond Doherty2, and L. A. Taylor1, 1Planetary Geoscience Institute, De- partment of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, 37996, USA, 24441 W Main Street, Tupelo, MS 38801, USA. Introduction: Enstatite chondrites are the rarest phosphides, and metal. Modal analyses of the two and most reduced chondrite clan [1]. E-chondrites are analyzed sections are given in Table 1. The subdivided into two groups, EL and EH, based on kamcite/silicate ratios of both sections are consistent modal iron-metal abundances. E-chondrites are charac- with EL chondrites. terized by the presence of nearly pure enstatite and silicon-bearing metal, with ferroan-alabandite in EL and niningerite in EH. Additionally, elements that are typically lithophilic in most meteorite groups (e.g., Mn, Mg, Ca, Na, K) can behave like chalcophile ele- ments in the E-chondrites due to the extremely reduc- ing conditions, forming a variety of accessory phases. Table 1. Modal analyses of Tupelo after [3]. * include graphite, Metamorphic characteristics used to define petrologic schreibersite, and all other non-sulfide, non-silicate minerals present. types [2] do not apply well to E-chondrites; therefore, **Troilite also includes alabandite and daubreelite. mineralogic types are utilized to specify metamorphic grade [3]. The silicates are nearly FeO-free enstatite (En98) The 280g Tupelo meteorite was found in 2012 by and sodic plagioclase feldspar (Ab77.7Or4.8). This feld- Maura O’Connell and Raymond Doherty, in a field in spar composition is consistent with composition re- Mississippi while looking for Indian artifacts. -
Fe,Mg)S, the IRON-DOMINANT ANALOGUE of NININGERITE
1687 The Canadian Mineralogist Vol. 40, pp. 1687-1692 (2002) THE NEW MINERAL SPECIES KEILITE, (Fe,Mg)S, THE IRON-DOMINANT ANALOGUE OF NININGERITE MASAAKI SHIMIZU§ Department of Earth Sciences, Faculty of Science, Toyama University, 3190 Gofuku, Toyama 930-8555, Japan § HIDETO YOSHIDA Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan § JOSEPH A. MANDARINO 94 Moore Avenue, Toronto, Ontario M4T 1V3, and Earth Sciences Division, Royal Ontario Museum, 100 Queens’s Park, Toronto, Ontario M5S 2C6, Canada ABSTRACT Keilite, (Fe,Mg)S, is a new mineral species that occurs in several meteorites. The original description of niningerite by Keil & Snetsinger (1967) gave chemical analytical data for “niningerite” in six enstatite chondrites. In three of those six meteorites, namely Abee and Adhi-Kot type EH4 and Saint-Sauveur type EH5, the atomic ratio Fe:Mg has Fe > Mg. Thus this mineral actually represents the iron-dominant analogue of niningerite. By analogy with synthetic MgS and niningerite, keilite is cubic, with space group Fm3m, a 5.20 Å, V 140.6 Å3, Z = 4. Keilite and niningerite occur as grains up to several hundred m across. Because of the small grain-size, most of the usual physical properties could not be determined. Keilite is metallic and opaque; in reflected light, it is isotropic and gray. Point-count analyses of samples of the three meteorites by Keil (1968) gave the following amounts of keilite (in vol.%): Abee 11.2, Adhi-Kot 0.95 and Saint-Sauveur 3.4. -
Magmatic Sulfides in the Porphyritic Chondrules of EH Enstatite Chondrites
Published in Geochimica et Cosmochimica Acta, Accepted September 2016. http://dx.doi.org/10.1016/j.gca.2016.09.010 Magmatic sulfides in the porphyritic chondrules of EH enstatite chondrites. Laurette Piani1,2*, Yves Marrocchi2, Guy Libourel3 and Laurent Tissandier2 1 Department of Natural History Sciences, Faculty of Science, Hokkaido University, Sapporo, 060-0810, Japan 2 CRPG, UMR 7358, CNRS - Université de Lorraine, 54500 Vandoeuvre-lès-Nancy, France 3 Laboratoire Lagrange, UMR7293, Université de la Côte d’Azur, CNRS, Observatoire de la Côte d’Azur,F-06304 Nice Cedex 4, France *Corresponding author: Laurette Piani ([email protected]) Abstract The nature and distribution of sulfides within 17 porphyritic chondrules of the Sahara 97096 EH3 enstatite chondrite have been studied by backscattered electron microscopy and electron microprobe in order to investigate the role of gas-melt interactions in the chondrule sulfide formation. Troilite (FeS) is systematically present and is the most abundant sulfide within the EH3 chondrite chondrules. It is found either poikilitically enclosed in low-Ca pyroxenes or scattered within the glassy mesostasis. Oldhamite (CaS) and niningerite [(Mg,Fe,Mn)S] are present in ! 60 % of the chondrules studied. While oldhamite is preferentially present in the mesostasis, niningerite associated with silica is generally observed in contact with troilite and low-Ca pyroxene. The Sahara 97096 chondrule mesostases contain high abundances of alkali and volatile elements (average Na2O = 8.7 wt.%, K2O = 0.8 wt.%, Cl = 7000 ppm and S = 3700 ppm) as well as silica (average SiO2 = 63.1 wt.%). Our data suggest that most of the sulfides found in EH3 chondrite chondrules are magmatic minerals that formed after the dissolution of S from a volatile-rich gaseous environment into the molten chondrules. -
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. -
Hydrated Minerals and Carbonaceous Chondrite Fragments in Lohawat Howardite: Astrobiological Implications: M
Astrobiology Science Conference 2015 (2015) 7069.pdf HYDRATED MINERALS AND CARBONACEOUS CHONDRITE FRAGMENTS IN LOHAWAT HOWARDITE: ASTROBIOLOGICAL IMPLICATIONS: M. S. Sisodia, A. Basu Sarbadhikari and R. R. Maha- jan. PLANEX, Physical Reasearch Laboratory, Ahmedabad, India (E-mail: [email protected]; [email protected]) Introduction: Presence of hydrated minerals on nebula caused initial melting and subsequent gradual asteroids, which are remnants of the blocks that formed differentiation of these early accreting bodies into the planets of the solar system has great importance for crust, mantle and core [4]. Dawn’s results confirm that deducing the origin of Earth’s water. Asteroid 4 Vesta Vesta is a differentiated protoplanet and that it is a is the parent body of the howardite-eucrite-diogenite parent body of HED meteorites [5]. The presence of (HED) family of the meteorites that have fallen on hydrated minerals on vesta as revealed by Lohawt Earth [1]. Lohawat howardite that fell in India in the howardite is very significant. Howardites originate year 1994 is a heterogeneous breccia composed of va- from the surface of Vesta nad constitute representative riety of mineral and lithic fragments [2]. We report samples from its crust, mantle and core. The low gravi- here optical study of hydrated minerals that we found ty of Vesta induce lower velocities to the impactors in Lohawat howardite and then discuss their astrobio- resulting into incomplete melting of impacting carbo- logical implications. naceous chondrites [6]. Whether these hydrated miner- Petrography of Lohawat howardite: Lohawat als were contributed on the surface of Vesta by carbo- howardite is an assortment of different minerals and naceous chondrites will be revealed by isotope study clasts. -
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. -
Carbonaceous Chondrite-Rich Howardites; the Potential for Hydrous Lithologies on the Hed Parent
CARBONACEOUS CHONDRITE-RICH HOWARDITES; THE POTENTIAL FOR HYDROUS LITHOLOGIES ON THE HED PARENT. J. S. Herrin 1,2 , M. E. Zolensky 2, J. A. Cartwright 3, D. W. Mittle- fehldt 2, and D. K. Ross 1,2 . 1ESCG Astromaterials Research Group, Houston, Texas, USA ( [email protected] ), 2NASA Johnson Space Center, Houston, Texas, USA, 3Max Planck Institut für Chemie, Mainz, Germany. Introduction: Howardites, eucrites, and dioge- clasts texturally resembling CM2 up to 7mm occupy- nites, collectively referred to as the “HED’s”, are a ing nearly half of the sample area accompanied 1-5 clan of meteorites thought to represent three different mm subangular impact melt clasts containing relict lithologies from a common parent body. Collectively eucritic fragments. The remaining medium and fine they are the most abundant type of achondrites in terre- fraction of the specimen consists of mm-to-sub-mm strial collections [1]. Eucrites are crustal basalts and angular-to-subrounded eucritic, diogenitic, carbona- gabbros, diogenites are mostly orthopyroxenites and ceous chondrite clasts set in a medium-to-coarse angu- are taken to represent lower crust or upper mantle ma- lar matrix of same materials. The eucrite/diogenite terials, and howardites are mixed breccias containing ratio of identifiable clasts is approximately 50/50. The both lithologies and are generally regarded as derived total modal abundance of visible carbonaceous chon- from the regolith or near-surface. drite fragments is ~60%. The presence of exogenous chondritic material in PRA 04402 is a howardite breccia consisting of howardite breccias has long been recognized [2,3]. As mm-to-sub-mm subrounded-to-subangular diogenite a group, howardites exhibit divergence in bulk chemi- and eucritic clasts in roughly equal proportions set in a stry from what would be produced by mixing of dioge- medium-to-coarse matrix. -
Geological Survey Canada
70-66 GEOLOGICAL PAPER 70-66 ., SURVEY OF CANADA DEPARTMENT OF ENERGY, MINES AND RESOURCES REVISED CATALOGUE OF THE NATIONAL METEORITE COLLECTION OF CANADA LISTING ACQUISITIONS TO AUGUST 31, 1970 J. A. V. Douglas 1971 Price, 75 cents GEOLOGICAL SURVEY OF CANADA CANADA PAPER 70-66 REVISED CATALOGUE OF THE NATIONAL METEORITE COLLECTION OF CANADA LISTING ACQUISITIONS TO AUGUST 31, 1970 J. A. V. Douglas DEPARTMENT OF ENERGY, MINES AND RESOURCES @)Crown Copyrights reserved Available by mail from Information Canada, Ottawa from the Geological Survey of Canada 601 Booth St., Ottawa and Information Canada bookshops in HALIFAX - 1735 Barrington Street MONTREAL - 1182 St. Catherine Street West OTTAWA - 171 Slater Street TORONTO - 221 Yonge Street WINNIPEG - 499 Portage Avenue VANCOUVER - 657 Granville Street or through your bookseller Price: 75 cents Catalogue No. M44-70-66 Price subject to change without notice Information Canada Ottawa 1971 ABSTRACT A catalogue of the National Meteorite Collection of Canada, published in 1963 listed 242 different meteorite specimens. Since then specimens from 50 a dditional meteorites have been added to the collection and several more specimens have been added to the tektite collection. This report describes all specimens in the collection. REVISED CATALOGUE OF THE NATIONAL METEORITE COLLECTION OF CANADA LISTING ACQUISITIONS TO AUGUST 31, 1970 INTRODUCTION At the beginning of the nineteenth century meteorites were recog nized as unique objects worth preserving in collections. Increasingly they have become such valuable objects for investigation in many fields of scienti fic research that a strong international interest in their conservation and pre servation has developed (c. f. -
1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. -
Sulfides in Enstate Chondrites
Sulfides in Enstatite Chondrites: Indicators of Impact History Kristyn Hill1,2, Emma Bullock2, Cari Corrigan2, and Timothy McCoy2 1Lock Haven University of Pennsylvania, Lock Haven, PA 17745, USA 2National Museum of Natural History, Department of Mineral Sciences, Washington D.C. 20013, USA Introductton Results Discussion Enstatite chondrites are a class of meteorites. They are Determining the history of the parent body of a referred to as chondrites because of the spherical Impact Melt, Slowly Cooled chondritic meteorite often includes distinguishing whether chondrules found in the matrix of the meteorites. Enstatite aa bb cc d d or not the meteorite was impact melted, and the cooling chondrites are the most highly reduced meteorites and rate. contain iron-nickel metal and sulfide bearing minerals. The Impact melts are distinguishable by the texture of the matrix is made up of silicates, enstatite in particular. There metal and sulfide assemblages. A meteorite that was are usually no oxides found, which supports the idea that impact melted will contain a texture of euhedral to these formed in very oxygen poor environments. The subhedral silicates, like enstatite, protruding into the metal enstatite chondrites in this study are type 3, meaning they or sulfides (figure 2). Some textures will look shattered are unmetamorphosed and not affected by fluids. (figure 2b). Meteorites that contain the mineral keilite are Studying enstatite chondrites will help us determine the PCA 91125 ALHA 77156 PCA 91444 PCA 91085 also an indicator of impact melts (figure 3). Keilite only evolution of their parent bodies which formed at the occurs in enstatite chondrite impact-melt rocks that cooled beginning of our solar system. -
Finegrained Precursors Dominate the Micrometeorite Flux
Meteoritics & Planetary Science 47, Nr 4, 550–564 (2012) doi: 10.1111/j.1945-5100.2011.01292.x Fine-grained precursors dominate the micrometeorite flux Susan TAYLOR1*, Graciela MATRAJT2, and Yunbin GUAN3 1Cold Regions Research and Engineering Laboratory, 72 Lyme Road, Hanover, New Hampshire 03755–1290, USA 2University of Washington, Seattle, Washington 98105, USA 3Geological & Planetary Sciences MC 170-25, Caltech, Pasadena, California 91125, USA *Corresponding author. E-mail: [email protected] (Received 15 May 2011; revision accepted 22 September 2011) Abstract–We optically classified 5682 micrometeorites (MMs) from the 2000 South Pole collection into textural classes, imaged 2458 of these MMs with a scanning electron microscope, and made 200 elemental and eight isotopic measurements on those with unusual textures or relict phases. As textures provide information on both degree of heating and composition of MMs, we developed textural sequences that illustrate how fine-grained, coarse-grained, and single mineral MMs change with increased heating. We used this information to determine the percentage of matrix dominated to mineral dominated precursor materials (precursors) that produced the MMs. We find that at least 75% of the MMs in the collection derived from fine-grained precursors with compositions similar to CI and CM meteorites and consistent with dynamical models that indicate 85% of the mass influx of small particles to Earth comes from Jupiter family comets. A lower limit for ordinary chondrites is estimated at 2–8% based on MMs that contain Na-bearing plagioclase relicts. Less than 1% of the MMs have achondritic compositions, CAI components, or recognizable chondrules. Single mineral MMs often have magnetite zones around their peripheries.