Part 1. Meteorites

Total Page:16

File Type:pdf, Size:1020Kb

Part 1. Meteorites Part 1. Meteorites GEOLOGICAL SURViTf PROFESSIONAL PAPER Data of Geochemistry Sixth Edition MICHAEL FLEISCHER, Technical Editor Chapter B. Cosmochemistry Part 1. Meteorites By BRIAN MASON GEOLOGICAL SURVEY PROFESSIONAL PAPER 440-B-l Tabulation and discussion of elemental abundances in the different classes of stony and iron meteorites, and in their constituent minerals UNITED STATES GOVERNMENT PRINTING OFFICE, WASHINGTON : 1979 UNITED STATES DEPARTMENT OF THE INTERIOR CECIL D. ANDRUS, Secretary GEOLOGICAL SURVEY H. William Menard, Director Library of Congress catalog-card No. 79-64561 For sale by the Superintendent of Documents, U.S. Government Printing Office Washington, D.C. 20402 Stock Number 024-001-031621 DATA OF GEOCHEMISTRY, SIXTH EDITION Michael Fleischer, Technical Editor The first edition of the Data of Geochemistry, by F. W. Clarke, was published in 1908 as U.S. Geological Survey Bulletin 330. Later editions, also by Clarke, were published in 1911, 1916, 1920, and 1924 as Bulletins 491, 616, 695, and 770. This, the sixth edition, has been written by several scientists in the Geological Survey and in other institutions in the United States and abroad, each preparing a chapter on his special field. The current edition is being published in individual chapters, titles of which are listed below. Chapters already published are indicated by boldface. CHAPTER A. The chemical elements B. Cosmochemistry Part 1, Meteorites by Brian Mason] Part 2, Cosmochemistry. C. Internal structure and composition of the earth. D. Composition of the earth's crust, by R. L. Parker E. Chemistry of the atmosphere F. Chemical composition of subsurface waters, by Donald E. White, John D. Hem, and G. A. Waring G. Chemical composition of rivers and lakes, by Daniel A. Livingstone H. Chemistry of the oceans I. Geochemistry of the biosphere J. Chemistry of rock-forming minerals K. Volcanic emanations, by Donald E. White and G. A. Waring L. Phase equilibrium relations of the common rock-forming oxides except water, by G. W. Morey M. Phase equilibrium relations of the common rock-forming oxides with water and (or) carbon dioxide N. Chemistry of igneous rocks, Part 1, The chemistry of the peralkaline oversaturated obsidians, by Bay Macdonald and D. K. Bailey 0. Chemistry of rock weathering and soils P. Chemistry of bauxites and laterites Q. Chemistry of nickel silicate deposits R. Chemistry of manganese oxides S. Chemical composition of sandstones excluding carbonate and volcanic sands, by F. J. Pettijohn T. Nondetrital siliceous sediments, by Earle R. Cressman U. Chemical composition of shales and related rocks V. Chemistry of carbonate rocks W. Chemistry of the iron-rich sedimentary rocks, by H. L. James X. Chemistry of phosphorites Y. Marine evaporites, by Frederick H. Stewart Z. Continental evaporites AA. Chemistry of coal BB. Chemistry of petroleum, natural gas, and miscellaneous carbonaceous substances CC. Chemistry of metamorphic rocks DD. Abundance and distribution of the chemical elements and their isotopes EE. Geochemistry of ore deposits FF. Physical chemistry of sulfide systems GG. The natural radioactive elements HH. Geochronology II. Temperatures of geologic processes JJ. Composition of fluid inclusions, by Edwin Roedder KK. Compilation of stable isotope fractionation factors of geochemical interest, by Irving Friedman and James R. O'Neil CONTENTS Page Page Abstract ________ Bl Germanium __________ . B53 Introduction __________ ____________ 1 Arsenic _________ 55 Historical background ___ ____________ 1 Selenium ____________ . 55 Phase composition of meteorites _ ____________ 2 Bromine ___________- . 57 Classification of meteorites _______ ___________ 4 Rubidium ____________ 60 Classification of chondrites _______________________ 4 Strontium ___________ - 60 Classification of achondrites and stony-irons _ 10 Yttrium ______________________ __ __ 64 Classification of iron meteorites __ .____________ 10 Zirconium ____________________ 64 Chemical fractionations in chondrites _____________ 13 Niobium _____________________. 65 The geochemical behavior of elements in meteorites 14 Molybdenum ___________________. 66 Location of minor and trace elements in meteorites 14 Ruthenium ___________________________ 67 Hydrogen ______ .______ 14 Rhodium _____________________________ 68 The noble gases: helium, neon, argon, krypton, xenon 16 Palladium ____________________._______ 69 Lithium ___________ _ .____________ 18 Silver ______________________________ 70 Beryllium ____________ .__________ 19 Cadmium ____________ ___ ._______ 71 Boron _____________ ___ ______ 20 Indium ______________________. 71 Carbon ________________________________ 20 Tin ________________________ 74 Nitrogen ____________ ___________ 21 Antimony ____________________________ 75 Oxygen .______ 23 Tellurium ____________________________ 76 Fluorine ____________________._________ 25 Iodine ______________________._______ 77 Sodium ________________________________ 26 Cesium _____________________. 78 Magnesium ____________ ___________ 29 Barium ______________________. 79 Aluminum _______________________________ 31 The lanthanides ____________ _________ 79 Silicon ______________________.__________ 33 Hafnium _____________________________ 86 Phosphorus __________________________ 34 Tantalum ____________________._______ 86 Sulfur ______________________.... 36 Tungsten _________________________ 87 Chlorine _____________ _______________ 37 Rhenium ____________________________ 88 Potassium ____________________________ 39 Osmium ___________ _ ._______ 89 Calcium _____________________________________________ 39 Iridium _____________________________ 90 Scandium ____________________.____________ 40 Platinum ____________________._______ 92 Titanium ____________________________________________ 41 Gold _______________________________ 94 Vanadium ___________________________________________ 44 Mercury _____________________________ 95 Chromium ___________________________________________ 44 Thallium ____________________._______ 97 Manganese __________________________________________ 45 Lead ___________________ 98 Iron _______________________.____________ 46 Bismuth _____________________._______ 100 Cobalt ______________________.____________ 49 Thorium _____________________________ 101 Nickel _______________________________________________ 50 Uranium ____________________________ 102 Copper __________________________________ 50 Conclusions ___________________________ 103 Zinc _______________________ ____________ 52 Acknowledgments _______________________ 123 Gallium _________________________________ 52 References cited ________________________ 123 ILLUSTRATIONS Page FIGURES 1-3. Graphs showing: 1. Relationship between elemental abundances in Type I carbonaceous chondrites and abundances in the Sun _______________ ___________________________ _______ B2 2. Relationship between oxidized iron and i ron as metal and sulfide in analyses of chondrites .___ 5 3. Relationship between CaO and FeO/(FeO+MgO) in the achondrites and stony-irons .______ 10 VI CONTENTS Page FIGURES 4-6. Diagrams showing 4. Relative abundances of selected elements in Type II and III carbonaceous chondrites and in ordinary chondrites, normalized to Type I carbonaceous chondrites=1.0 ___.____________ B13 5. Frequency distribution of carbon in chondrites _______________________.____________ 22 6. 0/ieO analyses of whole-rock samples and olivines from carbonaceous chondrites and whole-rock analyses of other meteorites ____ _________________________ ____________ 25 7. Graph showing relationship between Si02 and MgO in chondrites _______________._-_______ 31 8. Logarithmic plot showing Co-Ni distribution in meteorites __________ _ _ ._____ _ 50 9. Histogram showing the nickel content of analyzed iron meteorites _______________._________ 52 10-15. Logarithmic plots showing: 10. Ga-Ni distribution iron meteorites 57 11. Ge-Ni distribution iron meteorites 57 12. As-Ni distribution iron meteorites 60 13. Ru-Ni distribution in iron meteorites 69 14. Pd-Ni distribution in iron meteorites 71 15. Sb-Ni distribution in iron meteorites ___ _____________________.____________ 77 16,17. Diagrams showing: 16. Lanthanide abundances in Cl chondrites, C3 chondrites, and the eucrites (calcium-rich achon- drites ___________________________________.____________________ 84 17. Chondrite-normalized lanthanide abundances in achondrites _______ __ _ _____________ 85 18-22. Logarithmic plots showing: 18. Re-Ni distribution in iron meteorites 91 19. Os-Ni distribution in iron meteorites 91 20. Ir-Ni distribution in iron meteorites 94 21. Pt-Ni distribution in iron meteorites 94 22. Au-Ni distribution in iron meteorites 97 TABLES Page Page TABLE 1. The common minerals of meteorites ___ B2 15. Carbon in iron meteorites ______________ B22 2. Classification of meteorites ____________ 3 16. Nitrogen in stony meteorites __________ 23 3. Chemical analyses of chondritic meteorites __ 6 17. Nitrogen in iron meteorites ____________ 24 4. Petrologic types of chondrites _______ 9 18. Oxygen in stony meteorites ____________ 25 5. Classification of the chondrites _______ 10 19. Comparison of fluorine determinations 6. Structural classification of iron meteorites _ 11 chondrites _____________ 26 7. Structural and compositional properties of 20. Fluorine in stony meteorites __________ 27 iron meteorite groups ___________ 12 21. Sodium in stony meteorites ____________ 28 8. The geochemical behavior of the elements 30 in chondritic meteorites __________ 15 22. Magnesium in stony meteorites_________
Recommended publications
  • Handbook of Iron Meteorites, Volume 3
    Sierra Blanca - Sierra Gorda 1119 ing that created an incipient recrystallization and a few COLLECTIONS other anomalous features in Sierra Blanca. Washington (17 .3 kg), Ferry Building, San Francisco (about 7 kg), Chicago (550 g), New York (315 g), Ann Arbor (165 g). The original mass evidently weighed at least Sierra Gorda, Antofagasta, Chile 26 kg. 22°54's, 69°21 'w Hexahedrite, H. Single crystal larger than 14 em. Decorated Neu­ DESCRIPTION mann bands. HV 205± 15. According to Roy S. Clarke (personal communication) Group IIA . 5.48% Ni, 0.5 3% Co, 0.23% P, 61 ppm Ga, 170 ppm Ge, the main mass now weighs 16.3 kg and measures 22 x 15 x 43 ppm Ir. 13 em. A large end piece of 7 kg and several slices have been removed, leaving a cut surface of 17 x 10 em. The mass has HISTORY a relatively smooth domed surface (22 x 15 em) overlying a A mass was found at the coordinates given above, on concave surface with irregular depressions, from a few em the railway between Calama and Antofagasta, close to to 8 em in length. There is a series of what appears to be Sierra Gorda, the location of a silver mine (E.P. Henderson chisel marks around the center of the domed surface over 1939; as quoted by Hey 1966: 448). Henderson (1941a) an area of 6 x 7 em. Other small areas on the edges of the gave slightly different coordinates and an analysis; but since specimen could also be the result of hammering; but the he assumed Sierra Gorda to be just another of the North damage is only superficial, and artificial reheating has not Chilean hexahedrites, no further description was given.
    [Show full text]
  • Spring 1998 Gems & Gemology
    VOLUME 34 NO. 1 SPRING 1998 TABLE OF CONTENTS EDITORIAL 1 The Dr. Edward J. Gübelin Most Valuable Article Award FEATURE ARTICLE 4 The Rise to pProminence of the Modern Diamond Cutting Industry in India Menahem Sevdermish, Alan R. Miciak, and Alfred A. Levinson pg. 7 NOTES AND NEW TECHNIQUES 24 Leigha: The Creation of a Three-Dimensional Intarsia Sculpture Arthur Lee Anderson 34 Russian Synthetic Pink Quartz Vladimir S. Balitsky, Irina B. Makhina, Vadim I. Prygov, Anatolii A. Mar’in, Alexandr G. Emel’chenko, Emmanuel Fritsch, Shane F. McClure, Lu Taijing, Dino DeGhionno, John I. Koivula, and James E. Shigley REGULAR FEATURES pg. 30 44 Gem Trade Lab Notes 50 Gem News 64 Gems & Gemology Challenge 66 Book Reviews 68 Gemological Abstracts ABOUT THE COVER: Over the past 30 years, India has emerged as the dominant sup- plier of small cut diamonds for the world market. Today, nearly 70% by weight of the diamonds polished worldwide come from India. The feature article in this issue discuss- es India’s near-monopoly of the cut diamond industry, and reviews India’s impact on the worldwide diamond trade. The availability of an enormous amount of small, low-cost pg. 42 Indian diamonds has recently spawned a growing jewelry manufacturing sector in India. However, the Indian diamond jewelery–making tradition has been around much longer, pg. 46 as shown by the 19th century necklace (39.0 cm long), pendant (4.5 cm high), and bracelet (17.5 cm long) on the cover. The necklace contains 31 table-cut diamond panels, with enamels and freshwater pearls.
    [Show full text]
  • Mineralogy and Petrology of the Angrite Northwest Africa 1296 Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D
    Mineralogy and petrology of the angrite Northwest Africa 1296 Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D. Badia, C. Göpel, Marcel Bohn To cite this version: Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D. Badia, et al.. Mineralogy and petrology of the angrite Northwest Africa 1296. Meteoritics and Planetary Science, Wiley, 2005, 40 (3), pp.361-375. hal-00113853 HAL Id: hal-00113853 https://hal.archives-ouvertes.fr/hal-00113853 Submitted on 2 May 2011 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. Meteoritics & Planetary Science 40, Nr 3, 361–375 (2005) Abstract available online at http://meteoritics.org Mineralogy and petrology of the angrite Northwest Africa 1296 A. JAMBON,1 J. A. BARRAT,2 O. BOUDOUMA,3 M. FONTEILLES,4 D. BADIA,1 C. GÖPEL,5 and M. BOHN6 1Laboratoire Magie, Université Pierre et Marie Curie, CNRS UMR 7047, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 2UBO-IUEM, CNRS UMR 6538, Place Nicolas Copernic, F29280 Plouzané, France 3Service du MEB, UFR des Sciences de la Terre, Université Pierre et Marie Curie, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 4Pétrologie, Modélisation des Matériaux et Processus, Université Pierre et Marie Curie, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 5Laboratoire de Géochimie et Cosmochimie, Institut de Physique du Globe, CNRS UMR 7579, 4 place Jussieu, 75252 Paris cedex 05, France 6Ifremer-Centre de Brest, CNRS-UMR 6538, BP70, 29280 Plouzané Cedex, France *Corresponding author.
    [Show full text]
  • 19660017397.Pdf
    .. & METEORITIC RUTILE Peter R. Buseck Departments of Geology and Chemistry Arizona State University Tempe, Arizona Klaus Keil Space Sciences Division National Aeronautics and Space Administration Ames Research Center Mof fett Field, California r ABSTRACT Rutile has not been widely recognized as a meteoritic constituent. show, Recent microscopic and electron microprobe studies however, that Ti02 . is a reasonably widespread phase, albeit in minor amounts. X-ray diffraction studies confirm the Ti02 to be rutile. It was observed in the following meteorites - Allegan, Bondoc, Estherville, Farmington, and Vaca Muerta, The rutile is associated primarily with ilmenite and chromite, in some cases as exsolution lamellae. Accepted for publication by American Mineralogist . Rutile, as a meteoritic phase, is not widely known. In their sunanary . of meteorite mineralogy neither Mason (1962) nor Ramdohr (1963) report rutile as a mineral occurring in meteorites, although Ramdohr did describe a similar phase from the Faxmington meteorite in his list of "unidentified minerals," He suggested (correctly) that his "mineral D" dght be rutile. He also ob- served it in several mesosiderites. The mineral was recently mentioned to occur in Vaca Huerta (Fleischer, et al., 1965) and in Odessa (El Goresy, 1965). We have found rutile in the meteorites Allegan, Bondoc, Estherville, Farming- ton, and Vaca Muerta; although nowhere an abundant phase, it appears to be rather widespread. Of the several meteorites in which it was observed, rutile is the most abundant in the Farmington L-group chondrite. There it occurs in fine lamellae in ilmenite. The ilmenite is only sparsely distributed within the . meteorite although wherever it does occur it is in moderately large clusters - up to 0.5 mn in diameter - and it then is usually associated with chromite as well as rutile (Buseck, et al., 1965), Optically, the rutile has a faintly bluish tinge when viewed in reflected, plane-polarized light with immersion objectives.
    [Show full text]
  • Sulfide/Silicate Melt Partitioning During Enstatite Chondrite Melting
    61st Annual Meteoritical Society Meeting 5255.pdf SULFIDE/SILICATE MELT PARTITIONING DURING ENSTATITE CHONDRITE MELTING. C. Floss1, R. A. Fogel2, G. Crozaz1, M. Weisberg2, and M. Prinz2, 1McDonnell Center for the Space Sciences and Department of Earth and Planetary Sciences, Washington University, St. Louis MO 63130, USA ([email protected]), 2American Museum of Natural History, Department of Earth and Planetary Sciences, New York NY 10024, USA. Introduction: Aubrites are igneous rocks thought (present only in CaS-saturated charges) has a flat REE to have formed from an enstatite chondrite-like pattern with abundances of about 0.5 x CI. precursor [1]. Yet their origin remains poorly Discussion: Oldhamite/glass D values are close to understood, at least partly because of confusion over 1 for most REE, consistent with previous results the role played by sulfides, particularly oldhamite. [4,5,6], and significantly lower than those expected CaS in aubrites contains high rare earth element based on REE abundances in aubritic oldhamite. In (REE) abundances and exhibits a variety of patterns contrast, D values for FeS are surprisingly high (from [2] that reflect, to some extent, those seen in about 0.1 to 1), given the low REE abundances of oldhamite from enstatite chondrites [3]. However, natural troilite. FeS/silicate partition coefficients experimental work suggests that CaS/silicate melt reported by [5] are somewhat lower, but exhibit a REE partition coefficients are too low to account for similar pattern. Alkali loss from the charges, the high abundances observed [4,5] and do not explain resulting in Ca-enriched glass, might provide a partial the variable patterns.
    [Show full text]
  • Thursday, August 11, 2016 EARLY SOLAR SYSTEM CHRONOLOGY I 8:30 A.M
    79th Annual Meeting of the Meteoritical Society (2016) sess701.pdf Thursday, August 11, 2016 EARLY SOLAR SYSTEM CHRONOLOGY I 8:30 a.m. Room B Chairs: Gregory Brennecka Audrey Bouvier 8:30 a.m. Kruijer T. S. * Kleine T. Tungsten Isotope Dichotomy Among Iron Meteorite Parent Bodies: Implications for the Timescales of Accretion and Core Formation [#6449] We report new combined Pt and W isotope data for IC, IIC, IIF, IIIE, and IIIF iron meteorites, with the ultimate aim of better understanding the variable pre-exposure 182W/184W signatures observed among different iron meteorite groups. 8:45 a.m. Tissot F. L. H. * Dauphas N. Grove T. L. Heterogeneity in the 238U/235U Ratios of Angrites [#6104] We report the 238U/235U ratios of six angrites. We find that the angrite-parent body was heterogeneous with regards to U isotopes. We correct the Pb-Pb ages of angrites and test their concordance with ages derived from short-lived chronometers. 9:00 a.m. Brennecka G. A. * Amelin Y. Kleine T. Combined 238U/235U and Pb Isotopics of Planetary Core Material: The Absolute Age of the IVA Iron Muonionalusta [#6296] We report a measured 238U/235U for the IVA iron Muonionalusta. This measured value requires an age correction of ~7 Myr to the previously published Pb-Pb age. This has major implications for our understanding of planetary core formation and cooling. 9:15 a.m. Cartwright J. A. * Amelin Y. Koefoed P. Wadhwa M. U-Pb Age of the Ungrouped Achondrite NWA 8486 [#6231] We report the U-Pb age for ungrouped achondrite NWA 8486 (paired with NWA 7325).
    [Show full text]
  • 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.
    [Show full text]
  • Formation Mechanisms of Ringwoodite: Clues from the Martian Meteorite
    Zhang et al. Earth, Planets and Space (2021) 73:165 https://doi.org/10.1186/s40623-021-01494-1 FULL PAPER Open Access Formation mechanisms of ringwoodite: clues from the Martian meteorite Northwest Africa 8705 Ting Zhang1,2, Sen Hu1, Nian Wang1,2, Yangting Lin1* , Lixin Gu1,3, Xu Tang1,3, Xinyu Zou4 and Mingming Zhang1 Abstract Ringwoodite and wadsleyite are the high-pressure polymorphs of olivine, which are common in shocked meteorites. They are the major constituent minerals in the terrestrial mantle. NWA 8705, an olivine-phyric shergottite, was heavily shocked, producing shock-induced melt veins and pockets associated with four occurrences of ringwoodite: (1) the lamellae intergrown with the host olivine adjacent to a shock-induced melt pocket; (2) polycrystalline assemblages preserving the shapes and compositions of the pre-existing olivine within a shock-induced melt vein (60 μm in width); (3) the rod-like grains coexisting with wadsleyite and clinopyroxene within a shock-induced melt vein; (4) the microlite clusters embedded in silicate glass within a very thin shock-induced melt vein (20 μm in width). The frst two occurrences of ringwoodite likely formed via solid-state transformation from olivine, supported by their mor- phological features and homogeneous compositions (Mg# 64–62) similar to the host olivine (Mg# 66–64). The third occurrence of ringwoodite might fractionally crystallize from the shock-induced melt, based on its heterogeneous and more FeO-enriched compositions (Mg# 76–51) than those of the coexisting wadsleyite (Mg# 77–67) and the host olivine (Mg# 66–64) of this meteorite. The coexistence of ringwoodite, wadsleyite, and clinopyroxene suggests a post- shock pressure of 14–16 GPa and a temperature of 1650–1750 °C.
    [Show full text]
  • Handbook of Iron Meteorites, Volume 2 (Canyon Diablo, Part 2)
    Canyon Diablo 395 The primary structure is as before. However, the kamacite has been briefly reheated above 600° C and has recrystallized throughout the sample. The new grains are unequilibrated, serrated and have hardnesses of 145-210. The previous Neumann bands are still plainly visible , and so are the old subboundaries because the original precipitates delineate their locations. The schreibersite and cohenite crystals are still monocrystalline, and there are no reaction rims around them. The troilite is micromelted , usually to a somewhat larger extent than is present in I-III. Severe shear zones, 100-200 J1 wide , cross the entire specimens. They are wavy, fan out, coalesce again , and may displace taenite, plessite and minerals several millimeters. The present exterior surfaces of the slugs and wedge-shaped masses have no doubt been produced in a similar fashion by shear-rupture and have later become corroded. Figure 469. Canyon Diablo (Copenhagen no. 18463). Shock­ The taenite rims and lamellae are dirty-brownish, with annealed stage VI . Typical matte structure, with some co henite crystals to the right. Etched. Scale bar 2 mm. low hardnesses, 160-200, due to annealing. In crossed Nicols the taenite displays an unusual sheen from many small crystals, each 5-10 J1 across. This kind of material is believed to represent shock­ annealed fragments of the impacting main body. Since the fragments have not had a very long flight through the atmosphere, well developed fusion crusts and heat-affected rim zones are not expected to be present. The energy responsible for bulk reheating of the small masses to about 600° C is believed to have come from the conversion of kinetic to heat energy during the impact and fragmentation.
    [Show full text]
  • Magnetite Biomineralization and Ancient Life on Mars Richard B Frankel* and Peter R Buseckt
    Magnetite biomineralization and ancient life on Mars Richard B Frankel* and Peter R Buseckt Certain chemical and mineral features of the Martian meteorite with a mass distribution unlike terrestrial PAHs or those from ALH84001 were reported in 1996 to be probable evidence of other meteorites; thirdly, bacterium-shaped objects (BSOs) ancient life on Mars. In spite of new observations and up to several hundred nanometers long that resemble fos­ interpretations, the question of ancient life on Mars remains silized terrestrial microorganisms; and lastly, 10-100 nm unresolved. Putative biogenic, nanometer magnetite has now magnetite (Fe304), pyrrhotite (Fel_xS), and greigite (Fe3S4) become a leading focus in the debate. crystals. These minerals were cited as evidence because of their similarity to biogenic magnetic minerals in terrestrial Addresses magnetotactic bacteria. *Department of Physics, California Polytechnic State University, San Luis Obispo, California 93407, USA; e-mail: [email protected] The ancient life on Mars hypothesis has been extensively tDepartments of Geology and Chemistry/Biochemistry, Arizona State challenged, and alternative non-biological processes have University, Tempe, Arizona 85287-1404, USA; e-mail: [email protected] been proposed for each of the four features cited by McKay et al. [4]. In this paper we review the current situa­ tion regarding their proposed evidence, focusing on the Abbreviations putative biogenic magnetite crystals. BCM biologically controlled mineralization BIM biologically induced mineralization BSO bacterium-shaped object Evidence for and against ancient Martian life PAH polycyclic aromatic hydrocarbon PAHs and BSOs Reports of contamination by terrestrial organic materials [5°,6°] and the similarity of ALH84001 PAHs to non-bio­ genic PAHs in carbonaceous chondrites [7,8] make it Introduction difficult to positively identify PAHs of non-terrestrial, bio­ A 2 kg carbonaceous stony meteorite, designated genic origin.
    [Show full text]
  • 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,
    [Show full text]
  • Naretha Meteorite (Synonyms Kingoonya, Kingooya)
    Rec. West. Aust. Mus., 1976, 4 (1) NARETHA METEORITE (Sync;>nyms: Kingoonya, Kingooya) W.H. CLEVERLY* [Received 27 May 1975. Accepted 1 October 1975. Published 31 August 1976.1 ABSTRACT Much of the missing portion of the Naretha (Western Australia) meteorite has been located in museums as an un-named specimen and as two smaller specimens masquerading under the name 'Kingoonya' (or 'Kingooya'). The use of the junior synonyms with their implications of a South Australian site of find should be discontinued. INTRODUCfION Naretha meteorite, an L4 chondrite, was found in 1915 about 3 km north of the 205-mile station during construction of the Trans-Australian Railway. It was broken into at least three major pieces which were acquired by Mr John Darbyshire, Supervising Engineer for the construction of the western end of the railway (construction was proceeding simultaneously from both Kalgoorlie and Port Augusta ends - Fig. 1). Mr Darbyshire donated the meteorite to the W.A. School of Mines in Kalgoorlie where one' piece was retained and exhibited with a photograph of the reassembled meteorite (Fig. 2). A second fragment which was passed on to the Geological Survey of Western Australia was noted briefly by Simpson (1922) who first used the name 'Naretha', the name which had been given to the 205-mile station. There is strong presumptive evidence that the third fragment was passed on to Mr S.F.C. Cook of Kalgoorlie, a private collector from whose inaccurate verbal statements and undocumented collection, the subsequent confusion arose. In late 1926 Mr Cook gave a small piece of 'meteorite to Mr G.W.
    [Show full text]