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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. -
Constraints on the Water, Chlorine, and Fluorine Content of the Martian Mantle
Meteoritics & Planetary Science 1–13 (2016) doi: 10.1111/maps.12624 Constraints on the water, chlorine, and fluorine content of the Martian mantle 1* 2,3 4 Justin FILIBERTO , Juliane GROSS , and Francis M. MCCubbin 1Department of Geology, Southern Illinois University, 1259 Lincoln Dr, MC 4324, Carbondale, Illinois 62901, USA 2Department of Earth and Planetary Sciences, Rutgers University, 610 Taylor Road, Piscataway, New Jersey 08854, USA 3Department of Earth and Planetary Sciences, The American Museum of Natural History, New York, New York 10024, USA 4NASA Johnson Space Center, Mail Code XI2, 2101 NASA Parkway, Houston, Texas 77058, USA *Corresponding author. E-mail: fi[email protected] (Received 30 July 2015; revision accepted 22 January 2016) Abstract–Previous estimates of the volatile contents of Martian basalts, and hence their source regions, ranged from nearly volatile-free through estimates similar to those found in terrestrial subduction zones. Here, we use the bulk chemistry of Martian meteorites, along with Martian apatite and amphibole chemistry, to constrain the volatile contents of the Martian interior. Our estimates show that the volatile content of the source region for the Martian meteorites is similar to the terrestrial Mid-Ocean-Ridge Mantle source. Chlorine is enriched compared with the depleted terrestrial mantle but is similar to the terrestrial enriched source region; fluorine is similar to the terrestrial primitive mantle; and water is consistent with the terrestrial mantle. Our results show that Martian magmas were not volatile saturated; had water/chlorine and water/fluorine ratios ~0.4–18; and are most similar, in terms of volatiles, to terrestrial MORBs. Presumably, there are variations in volatile content in the Martian interior as suggested by apatite compositions, but more bulk chemical data, especially for fluorine and water, are required to investigate these variations. -
A Magnetic Susceptibility Database for Stony Meteorites
Direttore Enzo Boschi Comitato di Redazione Cesidio Bianchi Tecnologia Geofisica Rodolfo Console Sismologia Giorgiana De Franceschi Relazioni Sole-Terra Leonardo Sagnotti Geomagnetismo Giancarlo Scalera Geodinamica Ufficio Editoriale Francesca Di Stefano Istituto Nazionale di Geofisica e Vulcanologia Via di Vigna Murata, 605 00143 Roma Tel. (06) 51860468 Telefax: (06) 51860507 e-mail: [email protected] A MAGNETIC SUSCEPTIBILITY DATABASE FOR STONY METEORITES Pierre Rochette1, Leonardo Sagnotti1, Guy Consolmagno2, Luigi Folco3, Adriana Maras4, Flora Panzarino4, Lauri Pesonen5, Romano Serra6 and Mauri Terho5 1Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy [[email protected]] 2Specola Vaticana, Castel Gandolfo, Italy 3Antarctic [PNRA] Museum of Siena, Siena, Italy 4Università La Sapienza, Roma, Italy 5University of Helsinki, Finland 6“Giorgio Abetti” Museum of San Giovanni in Persiceto, Italy Pierre Rochette et alii: A Magnetic Susceptibility Database for Stony Meteorites 1. Introduction the Museo Nationale dell’Antartide in Siena [Folco and Rastelli, 2000], the University of More than 22,000 different meteorites Roma “la Sapienza” [Cavaretta Maras, 1975], have been catalogued in collections around the the “Giorgio Abetti” Museum in San Giovanni world (as of 1999) of which 95% are stony types Persiceto [Levi-Donati, 1996] and the private [Grady, 2000]. About a thousand new meteorites collection of Matteo Chinelatto. In particular, are added every year, primarily from Antarctic the Antarctic Museum in Siena is the curatorial and hot-desert areas. Thus there is a need for centre for the Antarctic meteorite collection rapid systematic and non-destructive means to (mostly from Frontier Mountain) recovered by characterise this unique sampling of the solar the Italian Programma Nazionale di Ricerche in system materials. -
CHAPTER 1 Introduction
Chemical analysis of organic molecules in carbonaceous meteorites Torrao Pinto Martins, Zita Carla Citation Torrao Pinto Martins, Z. C. (2007, January 24). Chemical analysis of organic molecules in carbonaceous meteorites. Retrieved from https://hdl.handle.net/1887/9450 Version: Corrected Publisher’s Version Licence agreement concerning inclusion of doctoral License: thesis in the Institutional Repository of the University of Leiden Downloaded from: https://hdl.handle.net/1887/9450 Note: To cite this publication please use the final published version (if applicable). ______________________________________________________ CHAPTER 1 ______________________________________________________ Introduction 1.1 Heavenly stones-from myth to science Ancient chronicles, from the Egyptian, Chinese, Greek, Roman and Sumerian civilizations documented the fall1 of meteorites, with Sumerian texts from around the end of the third millennium B. C. describing possibly one of the earliest words for meteoritic iron (Fig. 1.1 Left). Egyptian hieroglyphs meaning “heavenly iron” (Fig. 1.1 Right) found in pyramids together with the use of meteoritic iron in jewellery and artefacts show the importance of meteorites in early Egypt. Meteorites were worshiped by ancient Greeks and Romans, who struck coins to celebrate their fall, with the cult to worship meteorites prevailing for many centuries. For example, some American Indian tribes paid tribute to large iron meteorites, and even in modern days the Black Stone of the Ka´bah in Mecca is worshiped and regarded by Muslims as “an object from heaven”. The oldest preserved meteorite that was observed to fall (19th May 861) was found recently (October 1979) in a Shinto temple in Nogata, Japan. It weighted 472 g and it was stored in a wooden box. -
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. -
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. -
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. -
Subject Index.Fm
Meteoritics & Planetary Science 38, Nr 12, 1877–1878 (2003) http://meteoritics.org Annual Subject Index 26Al-26Mg relative ages 939 CM chondrites 813 Frictional melting 1521 26Mg excess 5 Coalescence 49 Geochemistry, brachinites 1601 40Ar-39Ar dating 555, 887 Cometary meteorites 1045 Geochemistry, Mars 1849 Ablation 1023 Comets 457, 1283 Grain 49 Accretion 1399 Cosmic dust flux 1351 Grain boundary 1669, 1679 Accretionary rims 813 Continuous flow isotope ratio mass Graphite 767 Acfer 182 spectrometer 1255 Hebe, asteroid 711 Achondrite(s) 95, 145, 157 Copernicus secondary craters 13 HH064 145 Achondrites, brachinites 1601 Complex impact structure 445 Hibonite 5 Achondrites, differentiated 1485 Core formation 1425 Hughes 030 5 Achondrites, primitive 1485 Cosmic-ray exposure ages 1243, 1485 Hydrated minerals 1383 Aenigmatite 725 Cosmic-ray exposure history 157 Hydrogen 357 Ages, 39Ar-40Ar 341, 1601 Cosmic spherules 329 Hydrothermal alteration 365 Airwave 989 Composition of meteorites 1005 Ice flow 1319 Albite 725 Cosmogenic nuclides 157 IDPs 1585 Allan Hills icefield 1319 Cratering 905 IDPs/chondrites 1283 ALH 84001 109, 849, 1697 Crater clusters 905 IIIAB Alkaline-rich clasts Crater fill deposits 1437 IIIAB iron meteorites 117 26Al 35 Creep 427 Impact 747 Amino acids 399 Cretaceous-tertiary boundary 1299 Impact basins 565 Amorphous carbon 767 Crust 895 Impact breccia 1079 Annealing 1499, 1507 Crustal magnetization 565 Impact crater(s) 1137, 1299, 1341, 1551 Antarctic meteorite(s) 109, 831 Cumulate(s) 529, 1753 Impact cratering 13, 1255, -
Thermal History of the Enstatite Chondrites from Silica Polymorphs
Meteoritics & Planetary Science 40, Nr 6, 855–868 (2005) Abstract available online at http://meteoritics.org Thermal history of the enstatite chondrites from silica polymorphs M. KIMURA1*, M. K. WEISBERG2, Y. LIN3, A. SUZUKI4, E. OHTANI4, and R. OKAZAKI5 1Faculty of Science, Ibaraki University, Mito 310-8512, Japan 2Department of Physical Sciences, Kingsborough College of the City University of New York, Brooklyn, New York 11235, and Department of Earth and Planetary Sciences, American Museum of Natural History, New York, New York 10024, USA 3State Key Laboratory of Lithosphere Tectonic Evolution, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China 4Institute of Mineralogy, Petrology, and Economic Geology, Graduate School of Science, Tohoku University, Sendai 980-8578, Japan 5Department of Earth and Planetary Sciences, Faculty of Sciences, Kyushu University, Fukuoka 812-8581, Japan *Corresponding author. E-mail: [email protected] (Received 18 January 2005; revision accepted 14 April 2005) Abstract–Here we report the results of our petrologic and mineralogical study of enstatite (E) chondrites in order to explore their thermal histories. We studied silica phases in 20 E chondrites by laser micro Raman spectroscopy to determine the silica polymorphs they contain. Silica phases are commonly present in E chondrites and their polymorphs reflect the physical conditions of formation. The samples studied here include EH3–5, EL3–6, E chondrite melt rocks, and an anomalous E chondrite. We identified quartz, tridymite, cristobalite, and silica glass in the samples studied. EH4– 5 and EH melt rocks are divided into high and low temperature classes based on niningerite- alabandite solid solutions. -
Meteorites: an Overview
Meteorites: An Overview Edward R. D. Scott* 1811-5209/11/0007-0047$2.50 DOI: 10.2113/gselements.7.1.47 eteorites come from numerous parent bodies with a wide variety chondrites are the most pristine, of geological histories. A few (~0.5%) come from Mars or the Moon; type 6 are the most metamor- phosed, and type 1 are the most Mthe rest are impact debris from collisions between asteroids orbiting aqueously altered. between Mars and Jupiter. Unlike terrestrial, Martian, and lunar rocks, the Asteroids that melted supply us asteroidal meteorites contain minerals that formed before the Sun and the with three major classes of mete- Solar System, during the growth of planetesimals and planets from the disk orites: irons, which are Fe–Ni of dust and gas around the Sun (“the solar nebula”), and during the first samples from the cores of aster- oids; metal-free silicate rocks from half-billion years of Solar System evolution. asteroidal mantles and crusts, Meteorites from unmelted asteroids are called chondrites; which are called achondrites as they are cosmic sediments composed of particles that were they lack chondrules; and stony irons, which are impact- generated mixtures of achondrites and Fe–Ni metal (Fig. present in the solar nebula (Fig. 1). The most abundant particles are millimeter-sized objects called chondrules, 2). Most irons (85%) are divided into thirteen groups which are solidified droplets of silicate magma. The chon- (called IAB, IIAB, IIC, etc.), which come from separate drules, associated grains of Fe–Ni metal, and a few volume parent bodies. The remaining ~15% probably come from percent or less of calcium–aluminum-rich inclusions another 50-odd parent bodies.