Revision 1 1 Transformation of Graphite to Lonsdaleite And

Total Page:16

File Type:pdf, Size:1020Kb

Revision 1 1 Transformation of Graphite to Lonsdaleite And Revision 1 1 Transformation of graphite to lonsdaleite and diamond in the Goalpara ureilite 2 directly observed by TEM 3 4 Yoshihiro Nakamuta1 and Shoichi Toh2 5 1University Museum, Kyushu University, Hakozaki, Fukuoka 812-8581, Japan 6 2HVEM Laboratory, Kyushu University, Motooka, Fukuoka 819-0395, Japan 7 8 ABSTRACT 9 Reflected-light microscopy and laser Raman spectroscopy of a polished thin section (PTS) 10 of the Goalpara ureilite and x-ray powder diffraction (XRPD) analyses of the grains taken 11 out of it elucidate the mode of occurrence of carbon grains which contain lonsdaleite and 12 diamond in the Goalpara ureilite. The results enable us to get samples with which precise 13 analyses can be made in order to know the formation mechanism of lonsdaleite and 14 diamond in ureilites. Selected area electron diffraction (SAED) analyses and high 15 resolution TEM (HRTEM) observations were carried out in the three unique directions of 16 pristine graphite with two thin slices prepared from a carbon grain directly taken out of a 17 PTS. SAED patterns reveal the relative crystal-axes orientations between graphite (Gr), 18 lonsdaleite (Lo) and diamond (Di) as (001)Gr // (100)Lo // (111)Di, [210]Gr // [001]Lo // [2-1- 19 1]Di and (1-20)Gr // (-120)Lo // (0-22)Di. The shapes of diffraction spots in the SAED patterns 20 reveal that the transformation of graphite to lonsdaleite is initiated by sliding of hexagonal 21 carbon planes of graphite along the [210] of graphite structure. These results suggest that 22 lonsdaleite and diamond in ureilites formed directly from graphite through boat-type 23 buckling and chair-type puckering of hexagonal carbon planes of graphite, respectively. 24 The results of this study confirm the shock origin of diamond in ureilites. 25 Keywords: Ureilite, graphite, lonsdaleite, diamond, transformation mechanism, TEM 1 Revision 1 26 INTRODUCTION 27 Diamond was found in the Novo Urei meteorite, one of typical ureilites, first in 28 meteorites in 1888 (Kunz, 1888). Lonsdaleite, hexagonal polymorph of diamond, was 29 found in the Canyon Diablo iron and the Goalpara ureilite first in nature (Bundy and Kasper, 30 1967; Frondel and Marvin, 1967; Hanneman et al., 1967). So far, mineralogical properties 31 of carbon minerals in ureilites have been only roughly determined by using acid-treatment 32 residues because they exist in small quantities in ureilites (Hanneman et al., 1967; Le 33 Guillou et al., 2010; Ringwood, 1960; Urey et al., 1957; Valter et al., 2003; Vdovykin, 34 1970). Then, the origin of diamonds in ureilites has been controversial (Arrhenius and 35 Alfvén, 1971; Fukunaga et al., 1987; Lipschutz, 1964; Urey, 1956). 36 Berkley and Jones (1982) reported that euhedral graphite blades occur without diamond 37 in the Allan Hills (ALH) 78019 ureilite. Euhedral tabular crystals of graphite were also 38 found in the Nova 001 and Nullarbor 010 ureilites and hard lumps in graphite crystals were 39 supposed to be diamond formed by shock (Treiman and Berkley, 1994). Nakamuta and 40 Aoki (2000) investigated carbon minerals in very weakly and weakly shocked ureilites and 41 observed blade-like shaped euhedral graphite crystals, being tan-grey color and bearing 42 metallic luster, in the very weakly shocked ALH 78019 and Yamato (Y)-82100 ureilites 43 with an optical microscope under a reflected light. They also observed blade-like shaped 44 grains in weakly shocked ureilites, Kenna, Y-79158 and ALH 77257, although these grains 45 are black in color and dull in luster. X-ray powder diffraction (XRPD) patterns of the grains 46 directly picked up from the polished thin section (PTS) of the Kenna ureilite reveal that the 47 grains are a mixture of graphite, compressed graphite and diamond. Lonsdaleite was not 2 Revision 1 48 found in these weakly shocked ureilites. The results suggest that diamond in ureilites was 49 formed from well-crystallized graphite having euhedral shapes by shock. In order to 50 confirm the origin of diamonds in ureilites and to elucidate the transformation mechanisms 51 of graphite to lonsdaleite and diamond, direct observation of structures of graphite, 52 lonsdaleite and diamond at the same area of a carbon grain is important but was not carried 53 out until now. The Goalpara ureilite is one of heavily shocked ureilites and is known to 54 contain lonsdaleite together with diamond (Hanneman et al., 1967). In this study, SAED 55 analyses and HRTEM observations were carried out in three directions with two slices 56 prepared from a carbon grain directly taken out of the PTS of the Goalpara ureilite and the 57 transformation mechanisms from graphite to lonsdaleite and diamond were proposed. 58 59 MATERIALS AND EXPERIMENTAL METHODS 60 The Goalpara ureilite is a monomict ureilite (Papike, 1998; Vdovykin, 1970). Urey et al. 61 (1957) found diamond in an acid-tretment residue of the meteorite based on an XRPD 62 analysis. Lonsdaleite was also found in an acid-tretment residue of the meteorite by an 63 XRPD analysis (Hanneman et al., 1967). 64 A PTS was prepared from a fragment of the Goalpara ureilite and observed by an optical 65 microscope. The meteorite mainly composed of coarse-grained olivine and pigeonite with 66 minor amounts of blade-like shaped carbon grains, being black in color and dull in luster 67 under a reflected light and up to 0.5 mm in size. Olivine and pyroxene crystals partly show 68 a mosaic texture, suggesting that the meteorite has been heavily shocked. Melting of 69 silicate minerals was not observed. 3 Revision 1 70 Micro Raman spectra of carbon grains in the PTS were recorded with a Jobin-Yvon 71 T64000 triple-grating spectrometer equipped with confocal optics and a nitrogen-cooled 72 CCD detector. A microscope was used to focus the 514.5 nm Ar exitation laser beam to a 1 73 µm spot. Accumulations lasting 120 seconds were made. The laser power on the sample 74 was 2 mW. 75 After micro Raman analyses, a typical carbon grain, a hundred µm in size, was removed 76 from the PTS and mounted on a glass fiber of ~10 µm in diameter for an XRPD analysis 77 using a 114 mm diameter Gandolfi camera (Gandolfi, 1967). A rotating anode x-ray 78 generator with a Cr-anode, 0.2 x 2 mm fine-filament, and a V-filter was used as an x-ray 79 source. The x-ray powder diffraction pattern was two-dimensionally recorded on an 80 imaging plate (IP), 35 mm wide and 350 mm long, and the intensity data on IP were read 81 by the 50 x 50 µm pixel size with a Fuji-film BAS-2500 IP-scanner. Intensities of 82 diffracted x-rays for each Bragg angle were obtained at intervals of 0.025º (2θ) by 83 averaging those along a Laue cone over 300 pixels of the central part of IP that had the 84 width of about 560 pixels. 85 SAED and HRTEM analyses were performed by using two thin slices of about 150 nm 86 thick which were prepared from the grain removed from a glass fiber used for the x-ray 87 analysis. FIB sample preparation was performed with a Ga ion beam by Hitachi FB-2000K 88 equipped with a micro-sampling unit at the Art, Science and Technology Center for 89 Cooperative Research, Kyushu University. One of the sides of the rectangular-shaped slice, 90 10 x 10 µm in size, was attached to the chipped edge of a copper disk of 3 mm in diameter 91 and set into TEM. SAED patterns and HRTEM imags were obtained by JEM-3200FSK 4 Revision 1 92 with a 300 kV accelerating voltage and a 400 mm camera length and recorded by a CCD 93 camera at the Research Laboratory for High Voltage Electron Microscopy of Kyushu 94 University. Diffraction patterns of Au were also obtained and used in order to correct d- 95 values of reflections of carbon minerals. 96 97 RESULTS 98 The mode of occurrence of carbon grains 99 Carbon grains occur along the grain boundaries of olivine with blade-like shapes (Fig. 100 1a). The rims of olivine crystals in contact with carbon grains include many tiny metal 101 blebs. The rims are thought to have been produced by redox reaction between olivine grains 102 and carbon when the parent body of ureilites has been break up (Goodrich, 1992; Goodrich 103 et al., 2004). The carbon grain, C1 in Figure 1a, was taken out of the PTS. The grain is 104 platy in shape with a thickness of 20 µm and a width of 100 x 100 µm (Fig. 1b). The shape 105 of the grain implies that the carbon grain has originally crystallized as a single crystal of 106 graphite (Berkley and Jones, 1982; Nakamuta and Aoki, 2000; Treiman and Berkley, 107 1994). 108 109 Raman spectroscopy 110 Raman spectra were measured at twenty points selected at random on the surface of the 111 C1 grain in the PTS (Fig. 1a). All spectra obtained are very similar to each other and show 112 a very broad Raman band spreading over the positions between 1200 and 1650 cm-1 and 113 high-fluorescence back ground (Fig. 2). The broad band has two peaks at around 1330 and 5 Revision 1 -1 -1 114 1590 cm , which may correspond to one-phonon band of diamond at 1332 cm and E2g 115 band of graphite at 1580 cm-1 (Hanfland et al., 1989), respectively. 116 117 XRPD analysis 118 An XRPD pattern was obtained by using the whole grain taken out of the PTS before 119 digging a hole to take a slice for TEM analysis.
Recommended publications
  • Experimental and Petrological Constraints on Lunar Differentiation from the Apollo 15 Green Picritic Glasses
    Meteoritics & Planetary Science 38, Nr 4, 515–527(2003) Abstract available online at http://meteoritics.org Experimental and petrological constraints on lunar differentiation from the Apollo 15 green picritic glasses Linda T. ELKINS-TANTON,1* Nilanjan CHATTERJEE,2 and Timothy L. GROVE2 1Department of Geological Sciences, Brown University, Providence, Rhode Island, 02912, USA 2Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA *Corresponding author: [email protected] (Received 15 July 2002; revision accepted 23 September 2002) Abstract–Phase equilibrium experiments on the most magnesian Apollo 15C green picritic glass composition indicate a multiple saturation point with olivine and orthopyroxene at 1520°C and 1.3 GPa (about 260 km depth in the moon). This composition has the highest Mg# of any lunar picritic glass and the shallowest multiple saturation point. Experiments on an Apollo 15A composition indicate a multiple saturation point with olivine and orthopyroxene at 1520°C and 2.2 GPa (about 440 km depth in the moon). The importance of the distinctive compositional trends of the Apollo 15 groups A, B, and C picritic glasses merits the reanalysis of NASA slide 15426,72 with modern electron microprobe techniques. We confirm the compositional trends reported by Delano (1979, 1986) in the major element oxides SiO2, TiO2, Al2O3, Cr2O3, FeO, MnO, MgO, and CaO, and we also obtained data for the trace elements P2O5, K2O, Na2O, NiO, S, Cu, Cl, Zn, and F. Petrogenetic modeling demonstrates that the Apollo 15 A-B-C glass trends could not have been formed by fractional crystallization or any continuous assimilation/fractional crystallization (AFC) process.
    [Show full text]
  • Lunar and Planetary Science XXX 1753.Pdf
    Lunar and Planetary Science XXX 1753.pdf INTERSTELLAR DIAMOND. II. GROWTH AND IDENTIFICATION. Andrew W. Phelps, University of Dayton Research Institute, Materials Engineering Division (300 College Park, Dayton OH, 45469-0130, [email protected]). likely form clumps of carbon that look much like the Introduction: The first abstract in this series starting material – hydrogen rich sp3 bound clusters. suggested that many types of diamond are found in many types of meteoritic material and that the The compounds that fit the requirements above variation in polytype abundance appears to reflect the include the cycloalkanes such as adamantane [21-30] nature of the host. How the diamonds got there and (C10H16) and bicyclooctane (C6H8) (BCO) . what they mean will now be examined. Opinions These compounds ‘look’ like small cubic diamonds regarding the formation mechanism(s) of meteoritic and lonsdaleite respectively. If these particular and interstellar diamond grains have changed over compounds are suggested as models for diamond the years as new methods of making synthetic nuclei then a number of structural and diamond were developed[1,2]. Meteoritic diamonds thermodynamic predictions can be made about the were once believed to be the result of high pressure - types of diamond that can form and its relative temperature processes in the interior of planetary abundance with regard to the physics and chemistry bodies[3,4]. Impact formation of diamond became of its growth environment. A few examples of this popular after the development of shock wave are: Adamantane is a lower energy form and would diamond synthesis[5] because shock synthesis was tend to form in an environment of sufficient thermal able to form lonsdaleite and meteorites were full of energy to allow the molecule to organize into this lonsdaleite.
    [Show full text]
  • Impact−Cosmic−Metasomatic Origin of Microdiamonds from Kumdy−Kol Deposit, Kokchetav Massiv, N
    11th International Kimberlite Conference Extended Abstract No. 11IKC-4506, 2017 Impact−Cosmic−Metasomatic Origin of Microdiamonds from Kumdy−Kol Deposit, Kokchetav Massiv, N. Kazakhstan L. I. Tretiakova1 and A. M. Lyukhin2 1St. Petersburg Branch Russian Mineralogical Society. RUSSIA, [email protected] 2Institute of remote ore prognosis, Moscow, RUSSIA, [email protected] Introduction Any collision extraterrestrial body and the Earth had left behind the “signature” on the Earth’s surface. We are examining a lot of signatures of an event caused Kumdy-Kol diamond-bearing deposit formation, best- known as “metamorphic” diamond locality among numerous UHP terrains around the world. We are offering new impact-cosmic-metasomatic genesis of this deposit and diamond origin provoked by impact event followed prograde and retrograde metamorphism with metasomatic alterations of collision area rocks that have been caused of diamond nucleation, growth and preserve. Brief geology of Kumdy-Kol diamond-bearing deposit Kumdy-Kol diamond-bearing deposit located within ring structure ~ 4 km diameter, in the form and size compares with small impact crater (Fig. 1). It is important impact event signature. Figure1: Cosmic image of Kumdy-Kol deposit area [http://map.google.ru/]. Diamond-bearing domain had been formed on the peak of UHP metamorphism provoked by comet impact under oblique angle on the Earth surface. As a result, steep falling system of tectonic dislocations, which breakage and fracture zones filling out of impact and host rock breccia with blastomylonitic and blastocataclastic textures have been created. Diamond-bearing domain has complicated lenticular-bloc structure (1300 x 40-200 m size) and lens out with deep about 300 m.
    [Show full text]
  • Chondrule Sizes, We Have Compiled and Provide Commentary on Available Chondrule Dimension Literature Data
    Invited review Chondrule size and related physical properties: a compilation and evaluation of current data across all meteorite groups. Jon M. Friedricha,b,*, Michael K. Weisbergb,c,d, Denton S. Ebelb,d,e, Alison E. Biltzf, Bernadette M. Corbettf, Ivan V. Iotzovf, Wajiha S. Khanf, Matthew D. Wolmanf a Department of Chemistry, Fordham University, Bronx, NY 10458 USA b Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024 USA c Department of Physical Sciences, Kingsborough College of the City University of New York, Brooklyn, NY 11235, USA d Graduate Center of the City University of New York, 365 5th Ave, New York, NY 10016 USA e Lamont-Doherty Earth Observatory, Columbia University, Palisades, New York 10964 USA f Fordham College at Rose Hill, Fordham University, Bronx, NY 10458 USA In press in Chemie der Erde – Geochemistry 21 August 2014 *Corresponding Author. Tel: +718 817 4446; fax: +718 817 4432. E-mail address: [email protected] 2 ABSTRACT The examination of the physical properties of chondrules has generally received less emphasis than other properties of meteorites such as their mineralogy, petrology, and chemical and isotopic compositions. Among the various physical properties of chondrules, chondrule size is especially important for the classification of chondrites into chemical groups, since each chemical group possesses a distinct size-frequency distribution of chondrules. Knowledge of the physical properties of chondrules is also vital for the development of astrophysical models for chondrule formation, and for understanding how to utilize asteroidal resources in space exploration. To examine our current knowledge of chondrule sizes, we have compiled and provide commentary on available chondrule dimension literature data.
    [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]
  • Lifetimes of Interstellar Dust from Cosmic Ray Exposure Ages of Presolar Silicon Carbide
    Lifetimes of interstellar dust from cosmic ray exposure ages of presolar silicon carbide Philipp R. Hecka,b,c,1, Jennika Greera,b,c, Levke Kööpa,b,c, Reto Trappitschd, Frank Gyngarde,f, Henner Busemanng, Colin Madeng, Janaína N. Ávilah, Andrew M. Davisa,b,c,i, and Rainer Wielerg aRobert A. Pritzker Center for Meteoritics and Polar Studies, The Field Museum of Natural History, Chicago, IL 60605; bChicago Center for Cosmochemistry, The University of Chicago, Chicago, IL 60637; cDepartment of the Geophysical Sciences, The University of Chicago, Chicago, IL 60637; dNuclear and Chemical Sciences Division, Lawrence Livermore National Laboratory, Livermore, CA 94550; ePhysics Department, Washington University, St. Louis, MO 63130; fCenter for NanoImaging, Harvard Medical School, Cambridge, MA 02139; gInstitute of Geochemistry and Petrology, ETH Zürich, 8092 Zürich, Switzerland; hResearch School of Earth Sciences, The Australian National University, Canberra, ACT 2601, Australia; and iEnrico Fermi Institute, The University of Chicago, Chicago, IL 60637 Edited by Mark H. Thiemens, University of California San Diego, La Jolla, CA, and approved December 17, 2019 (received for review March 15, 2019) We determined interstellar cosmic ray exposure ages of 40 large ago. These grains are identified as presolar by their large isotopic presolar silicon carbide grains extracted from the Murchison CM2 anomalies that exclude an origin in the Solar System (13, 14). meteorite. Our ages, based on cosmogenic Ne-21, range from 3.9 ± Presolar stardust grains are the oldest known solid samples 1.6 Ma to ∼3 ± 2 Ga before the start of the Solar System ∼4.6 Ga available for study in the laboratory, represent the small fraction ago.
    [Show full text]
  • 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.
    [Show full text]
  • Addibischoffite, Ca2al6al6o20, a New Calcium Aluminate Mineral from The
    1 Revision 3 2 Addibischoffite, Ca2Al6Al6O20, a new calcium aluminate mineral from 3 the Acfer 214 CH carbonaceous chondrite: A new refractory phase from 4 the solar nebula 5 Chi Ma1,*, Alexander N. Krot2, Kazuhide Nagashima2 6 1Division of Geological and Planetary Sciences, California Institute of Technology, 7 Pasadena, California 91125, USA 8 2Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, 9 Honolulu, Hawai‘i 96822, USA 10 11 ABSTRACT 12 Addibischoffite (IMA 2015-006), Ca2Al6Al6O20, is a new calcium aluminate mineral 13 that occurs with hibonite, perovskite, kushiroite, Ti-kushiroite, spinel, melilite, 14 anorthite and FeNi-metal in the core of a Ca-Al-rich inclusion (CAI) in the Acfer 15 214 CH3 carbonaceous chondrite. The mean chemical composition of type 16 addibischoffite by electron probe microanalysis is (wt%) Al2O3 44.63, CaO 15.36, 17 SiO2 14.62, V2O3 10.64, MgO 9.13, Ti2O3 4.70, FeO 0.46, total 99.55, giving rise to 18 an empirical formula of 3+ 3+ 2+ 19 (Ca2.00)(Al2.55Mg1.73V 1.08Ti 0.50Ca0.09Fe 0.05)Σ6.01(Al4.14Si1.86)O20. The general 20 formula is Ca2(Al,Mg,V,Ti)6(Al,Si)6O20. The end-member formula is Ca2Al6Al6O20. 21 Addibischoffite has the P1 aenigmatite structure with a = 10.367 Å, b = 10.756 Å, c 22 = 8.895 Å, α = 106.0°, β = 96.0°, γ = 124.7°, V = 739.7 Å3, and Z = 2, as revealed by 23 electron back-scatter diffraction. The calculated density using the measured 24 composition is 3.41 g/cm3.
    [Show full text]
  • POSTER SESSION 5:30 P.M
    Monday, July 27, 1998 POSTER SESSION 5:30 p.m. Edmund Burke Theatre Concourse MARTIAN AND SNC METEORITES Head J. W. III Smith D. Zuber M. MOLA Science Team Mars: Assessing Evidence for an Ancient Northern Ocean with MOLA Data Varela M. E. Clocchiatti R. Kurat G. Massare D. Glass-bearing Inclusions in Chassigny Olivine: Heating Experiments Suggest Nonigneous Origin Boctor N. Z. Fei Y. Bertka C. M. Alexander C. M. O’D. Hauri E. Shock Metamorphic Features in Lithologies A, B, and C of Martian Meteorite Elephant Moraine 79001 Flynn G. J. Keller L. P. Jacobsen C. Wirick S. Carbon in Allan Hills 84001 Carbonate and Rims Terho M. Magnetic Properties and Paleointensity Studies of Two SNC Meteorites Britt D. T. Geological Results of the Mars Pathfinder Mission Wright I. P. Grady M. M. Pillinger C. T. Further Carbon-Isotopic Measurements of Carbonates in Allan Hills 84001 Burckle L. H. Delaney J. S. Microfossils in Chondritic Meteorites from Antarctica? Stay Tuned CHONDRULES Srinivasan G. Bischoff A. Magnesium-Aluminum Study of Hibonites Within a Chondrulelike Object from Sharps (H3) Mikouchi T. Fujita K. Miyamoto M. Preferred-oriented Olivines in a Porphyritic Olivine Chondrule from the Semarkona (LL3.0) Chondrite Tachibana S. Tsuchiyama A. Measurements of Evaporation Rates of Sulfur from Iron-Iron Sulfide Melt Maruyama S. Yurimoto H. Sueno S. Spinel-bearing Chondrules in the Allende Meteorite Semenenko V. P. Perron C. Girich A. L. Carbon-rich Fine-grained Clasts in the Krymka (LL3) Chondrite Bukovanská M. Nemec I. Šolc M. Study of Some Achondrites and Chondrites by Fourier Transform Infrared Microspectroscopy and Diffuse Reflectance Spectroscopy Semenenko V.
    [Show full text]
  • Impact Shock Origin of Diamonds in Ureilite Meteorites
    Impact shock origin of diamonds in ureilite meteorites Fabrizio Nestolaa,b,1, Cyrena A. Goodrichc,1, Marta Moranad, Anna Barbarod, Ryan S. Jakubeke, Oliver Christa, Frank E. Brenkerb, M. Chiara Domeneghettid, M. Chiara Dalconia, Matteo Alvarod, Anna M. Fiorettif, Konstantin D. Litasovg, Marc D. Friesh, Matteo Leonii,j, Nicola P. M. Casatik, Peter Jenniskensl, and Muawia H. Shaddadm aDepartment of Geosciences, University of Padova, I-35131 Padova, Italy; bGeoscience Institute, Goethe University Frankfurt, 60323 Frankfurt, Germany; cLunar and Planetary Institute, Universities Space Research Association, Houston, TX 77058; dDepartment of Earth and Environmental Sciences, University of Pavia, I-27100 Pavia, Italy; eAstromaterials Research and Exploration Science Division, Jacobs Johnson Space Center Engineering, Technology and Science, NASA, Houston, TX 77058; fInstitute of Geosciences and Earth Resources, National Research Council, I-35131 Padova, Italy; gVereshchagin Institute for High Pressure Physics RAS, Troitsk, 108840 Moscow, Russia; hNASA Astromaterials Acquisition and Curation Office, Johnson Space Center, NASA, Houston, TX 77058; iDepartment of Civil, Environmental and Mechanical Engineering, University of Trento, I-38123 Trento, Italy; jSaudi Aramco R&D Center, 31311 Dhahran, Saudi Arabia; kSwiss Light Source, Paul Scherrer Institut, 5232 Villigen, Switzerland; lCarl Sagan Center, SETI Institute, Mountain View, CA 94043; and mDepartment of Physics and Astronomy, University of Khartoum, 11111 Khartoum, Sudan Edited by Mark Thiemens, University of California San Diego, La Jolla, CA, and approved August 12, 2020 (received for review October 31, 2019) The origin of diamonds in ureilite meteorites is a timely topic in to various degrees and in these samples the graphite areas, though planetary geology as recent studies have proposed their formation still having external blade-shaped morphologies, are internally at static pressures >20 GPa in a large planetary body, like diamonds polycrystalline (18).
    [Show full text]
  • I-Xe Analysis of Enstatite Meteorites and a Eucrite
    Testing an integrated chronology: I-Xe analysis of enstatite meteorites and a eucrite Item Type Article; text Authors Busfield, A.; Turner, G.; Gilmour, J. D. Citation Busfield, A., Turner, G., & Gilmour, J. D. (2008). Testing an integrated chronology: IXe analysis of enstatite meteorites and a eucrite. Meteoritics & Planetary Science, 43(5), 883-897. DOI 10.1111/j.1945-5100.2008.tb01087.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 26/09/2021 21:32:45 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656429 Meteoritics & Planetary Science 43, Nr 5, 883–897 (2008) AUTHOR’S PROOF Abstract available online at http://meteoritics.org Testing an integrated chronology: I-Xe analysis of enstatite meteorites and a eucrite A. BUSFIELD, G. TURNER, and J. D. GILMOUR* School of Earth, Atmospheric and Environmental Science, University of Manchester, Oxford Road, Manchester M13 9PL, UK *Corresponding author. E-mail: [email protected] (Supplementary tables and figures are available online at http://meteoritics.org/online supplements.htm) (Received 06 October 2006; revision accepted 21 November 2007) Abstract–We have determined initial 129I/127I ratios for mineral concentrates of four enstatite meteorites and a eucrite. In the case of the enstatite meteorites the inferred ages are associated with the pyroxene-rich separates giving pyroxene closure ages relative to the Shallowater standard of Indarch (EH4, 0.04 ± 0.67 Ma), Khairpur (EL6, −4.22 ± 0.67 Ma), Khor Temiki (aubrite, −0.06 Ma), and Itqiy (enstatite achondrite, −2.6 ± 2.6 Ma), negative ages indicate closure after Shallowater.
    [Show full text]
  • Petrography and Mineral Chemistry of the Anhydrous Component of the Tagish Lake Carbonaceous Chondrite
    Meteoritics & Planetary Science 38, Nr 5, 813–825 (2003) Abstract available online at http://meteoritics.org Petrography and mineral chemistry of the anhydrous component of the Tagish Lake carbonaceous chondrite S. B. SIMON1* and L. GROSSMAN1, 2 1Department of the Geophysical Sciences, 5734 South Ellis Avenue, The University of Chicago, Chicago, Illinois 60637, USA 2The Enrico Fermi Institute, 5640 South Ellis Avenue, The University of Chicago, Chicago, Illinois 60637, USA *Corresponding author. E-mail: [email protected] (Received 30 August 2002; revision accepted 16 January 2003) Abstract–Most studies of Tagish Lake have considered features that were either strongly affected by or formed during the extensive hydrous alteration experienced by this meteorite. This has led to some ambiguity as to whether Tagish Lake should be classified a CI, a CM, or something else. Unlike previous workers, we have focused upon the primary, anhydrous component of Tagish Lake, recovered through freeze-thaw disaggregation and density separation and located by thin section mapping. We found many features in common with CMs that are not observed in CIs. In addition to the presence of chondrules and refractory forsterite (which distinguish Tagish Lake from the CIs), we found hibonite-bearing refractory inclusions, spinel-rich inclusions, forsterite aggregates, Cr-, Al-rich spinel, and accretionary mantles on many clasts, which clearly establishes a strong link between Tagish Lake and the CM chondrites. The compositions of isolated olivine crystals in Tagish Lake are also like those found in CMs. We conclude that the anhydrous inclusion population of Tagish Lake was, originally, very much like that of the known CM chondrites and that the inclusions in Tagish Lake are heavily altered, more so than even those in Mighei, which are more heavily altered than those in Murchison.
    [Show full text]