DOCSLIB.ORG

The Meteoritical Bulletin, No. 103 ALEX RUZICKA1, JEFFREY GROSSMAN2, AUDREY BOUVIER3, and CARL B

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Meteoritical Bulletin, No. 103 ALEX RUZICKA1, JEFFREY GROSSMAN2, AUDREY BOUVIER3, and CARL B The Meteoritical Bulletin, No. 103 ALEX RUZICKA1, JEFFREY GROSSMAN2, AUDREY BOUVIER3, and CARL B. AGEE4 1Cascadia Meteorite Laboratory, Department of Geology, Portland State University, Portland, Oregon, 97207-0751, USA 2U.S. Geological Survey, MS 954, Reston, Virginia 20192, USA 3Western University, Department of Earth Sciences, London, Ontario, N6A B57, Canada 4Institute of Meteoritics, Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, New Mexico, 87131-0001, USA Abstract: Meteoritical Bulletin 103 contains 2582 meteorites including 10 falls (Ardón, Demsa, Jinju, Križevci, Kuresoi, Novato, Tinajdad, Tirhert, Vicência, Wolcott), with 2174 Ordinary chondrites, 130 HED achondrites, 113 Carbonaceous chondrites, 41 Ureilites, 27 Lunar meteorites, 24 Enstatite chondrites, 21 Iron meteorites, 15 Primitive achondrites, 11 Mesosiderites, 10 Martian meteorites, 6 Rumuruti chondrites, 5 Ungrouped achondrites, 2 Enstatite achondrites, 1 Relict meteorite, 1 Pallasite, and 1 Angrite, and with 1511 from Antarctica, 588 from Africa, 361 from Asia, 86 from South America, 28 from North America, and 6 from Europe. Note: 1 meteorite from Russia was counted as European. The complete contents of this bulletin (244 pages) are available on line. Information about approved meteorites can be obtained from the Meteoritical Bulletin Database (MBD) available on line at http://www.lpi.usra.edu/meteor/ . Table of Contents 1. Alphabetical text entries for non-Antarctic meteorites ..………………………………………1 2. Bibliography ……………………..……………………………………………………….... 180 3. Alphabetical listing of all meteorites ..………..……………………………………………..181 4. Corrected entries ………………..…………………………………………………………...240 5. Listing of institutes and collections …..……………………………………………………..240 6. Acknowledgments …………………..………………………………………………………243 1 1. Alphabetical text entries for non-Antarctic meteorites Abar al’ Uj 012 (AaU 012) 22°23.999’N, 48°42.409’E Ash Sharqiyah, Saudi Arabia Found: 31 Jan 2012 Classification: Lunar meteorite History: Found by Edwin Gnos, Beda Hofmann, Khalid al Wagdani, Ayman Majoub, Abdulaziz Solami, Siddiq Habibullah, Maruan Al Bokari during a search for meteorites on January 31, 2012. Physical characteristics: Medium gray stone with a total mass of 122.78 g. The wind-ablated meteorite consists of two fitting fragments, with masses of 104.5 and 18.27 g, respectively. Fusion crust is absent. Contains black, white and red mineral and lithic clasts (up to 6 mm) embedded in a very fine-grained matrix. Vesicles are abundant. Some vesicles and thin cracks are filled with terrestrial mineral assemblages. Petrography: (B. Hofmann NMBE; M. Mészáros NMBE/Bern) Clast-rich impact-melt breccia, consisting of partly resorbed mineral clasts (up to 1 mm) and subrounded/rounded lithic clasts (up to 6.8 mm) set in a very fine-grained, well-crystallized impact-melt matrix. Most common mineral clasts are plagioclase with minor pyroxene and olivine. The lithic clast population is dominated by anorthositic breccias. Rare clasts of igneous rocks and a single basalt clast were observed. Vesicles (up to 3.0 mm diameter) are abundant. Shock features (polycrystalline grains, mosaicism, recrystallization) were observed in pyroxenes, olivine and plagioclase. Trace mineral phases are troilite, FeNi-metal, spinel (pleonast), SiO2 and terrestrial alteration products (carbonates, celestine, Fe-hydroxides). Geochemistry: (N. Greber, M. Mészáros, Bern) Mineral composition: feldspar (n=46): An93.4-97.7 Or0.0-1.6; olivine (n=7): Fa28.4-35.3, Fe/Mn=95.7; orthopyroxene (n=1): Wo3.6 Fs25.2, Fe/Mn=52.8; clinopyroxene (n=10): Wo5.1-40.6 Fs12.8-36.9, Fe/Mn=89.9. Bulk analysis (ICP/ICPMS): Al2O3=28.9 wt%, FeO=5.0 wt%, Sc=8 ppm, Sm=1.2 ppm, Th=0.5 ppm. Oxygen isotopes: (R. Greenwood, OU): δ18O=5.46 permil, δ17O=2.86 permil Δ17O=0.018 permil. Classification: Lunar feldspathic impact-melt breccia. Specimens: Type material (25.1 g) and 3 polished thin sections at MHNGE, main mass at SGS. Abar al’ Uj 014 (AaU 014) 22°26.380’N, 48°52.250’E Ash Sharqiyah, Saudi Arabia Found: 31 Jan 2012 Classification: Carbonaceous chondrite (CO3) History: Found by Edwin Gnos, Beda Hofmann, Khalid al Wagdani, Ayman Majoub, Abdulaziz Solami, Siddiq Habibullah, Maruan Al Bokari during a search for meteorites on Jan. 31, 2012. Physical characteristics: Dark brown, wind-ablated, partially broken 429.4 g individual, no preserved fusion crust. Petrography: (E. Gnos, MHNGE and B. Hofmann, NMBE) Abundant chondrules (approx. 60% vol), matrix approx. 40% vol. CAIs up to 500 μm. Chondrule size averages 0.28±0.14 mm (n= 180, maximum size 0.90 mm). Chondrules commonly contain brown glass. Abundant troilite and iron metal (approx. 5:1). Shock grade S1. Weathering: about 50% of metal is oxidized. Geochemistry: Olivine compositions are Fa0.5-56.5, median Fa35.5 (n=72), pyroxene compositions are Fs0.0- 18 17 22.1Wo0.5-6.2, median Fs2.6Wo1.4 (n=19). Oxygen isotopes: (R. Greenwood, OU) gave δ O = -0.14, δ O = - 4.59, Δ17O = -4.52 (all permil) Classification: Based on Chondrule size, matrix abundance and geochemistry this is a CO3 chondrite. Specimens: Type material (21.70 g) and three polished thin sections at MHNGE, main mass at SGS. Al Hawaya 002 19°50.603’N, 49°11.197’E Ash Sharqiyah, Saudi Arabia Found: 15 Feb 2013 Classification: Ureilite 2 History: Found by Edwin Gnos, Beda Hofmann, Ayman Majoub search for meteorites on small patch of desert soil between dunes on Feb. 15, 2013. Physical characteristics: Dark brown, wind-polished broken individual of 7.61 g. Strongly weathered. Petrography: Polished thin section shows typical ureilitic texture with interlocked olivine and pyroxene grains typically 1 mm in size, with undulose extinction. Carbon platelets are very common (~10 vol%) and consist mainly of diamond. Metal and troilite are largely oxidized, only few remnant inclusions in silicates. Silicates are partly affected by terrestrial alteration. Geochemistry: (N. Greber, Bern) Olivine compositions are Fa10.2-21.8, median Fa21.4, median Cr2O3 0.49 wt% (n=29), pyroxene compositions are Fs7.2-18.3Wo4.7-22.1, median Fs14.4Wo10.7, median Cr2O3 1.25 wt% (n=8). Bulk analysis of cut surface by XRF (wt%): Fe 17.0, Mn 0.28 (Fe/Mn 60.4), Ni 0.16, Cr 0.53. Classification: Based on texture, silicate compositions and abundant diamond platelets this is a ureilite. Specimens: 2.28 g and one polished thin section at MHNGE. Remaining material SGS. Al Hawaya 004 19°47.634’N, 49°09.605’E Ash Sharqiyah, Saudi Arabia Found: 16 Feb 2013 Classification: HED achondrite (Eucrite, polymict) History: Found by Abu Badr al Obeidi during a search for meteorites on small patch of sandy soil between dunes on February 16, 2013. Physical characteristics: Wind-polished individual with a total mass of 176.9 g, showing partial brecciated texture, no fusion crust preserved. Petrography: Breccia containing a variety of basaltic lithologies, generally plagioclase-rich with lath-like plagioclase typically 0.5-0.9 mm long, and some pyroxene laths up to 1.8 mm. A silica phase is commonly present. A macroscopically dark grey, fine-grained clast (mean grain size 5-10 μm) with equilibrated metamorphic texture also contains silica phase. Accessories are ilmenite, magnetite, troilite and rare iron metal. Geochemistry: (N. Greber, Bern) Orthopyroxene compositions are Fs55.0-60.2Wo1.7-8.4, median Fs56.9Wo5.2 (n=12). Clinopyroxene compositions are Fs27.7-53.2Wo10.5-41.5, median Fs42.4Wo22.7 (n=4). Plagioclase: An92.2Or0.3 (n=1). Bulk analysis of cut surface by XRF (wt%): Fe 14.6, Mn 0.43 (Fe/Mn 34.2). Oxygen isotopes: (R. Greenwood, OU) gave δ18O = 3.93, δ17O = 1.82, Δ17O = -0.226 (all per mil). Classification: Based on texture, mineral composition, oxygen isotopes and bulk Fe/Mn this is a eucrite (basaltic eucrite breccia). Specimens: 31.66 g and one polished thin section at MHNGE. Remaining material SGS. Al Hawaya 010 19°30.068’N, 48°01.808’E Ash Sharqiyah, Saudi Arabia Found: 16 Feb 2013 Classification: Ureilite History: Found by Hassan Al Marsouki during search for meteorites on small patch of desert soil between dunes on February 14, 2013. Physical characteristics: Dark brown fragment of 3.91 g, partially covered by cemented dune sand. Petrography: Polished thin section shows typical ureilitic texture with interlocked olivine (~25 vol%) and pyroxene (~70 vol%) grains 0.8-1.6 mm in size. Common graphite crystals up to 1 mm (~5 vol%), no diamond observed. Metal is largely oxidized, only few remnant inclusions in silicates. Graphite shows only minor deformation. Olivine is partly affected by terrestrial alteration. Geochemistry: (N. Greber, Bern) Olivine compositions are Fa12.0-13.2, median Fa12.3 (n=14), pyroxene compositions are Fs10.4-11.0Wo4.7-4.9, median Fs10.6Wo4.8 (n=15). Silicates are Cr-rich (0.49±0.16 wt% in olivine, 0.95±0.32 wt% in pyroxene). Bulk analysis of cut surface by XRF (wt%): Fe 13.3, Mn 0.38 (Fe/Mn 35.0), Ni 0.23, Cr 0.64. Classification: Based on texture, silicate compositions and abundant graphite this is a ureilite. Specimens: 1.33 g and one polished thin section at MHNGE. Remaining material SGS. 3 Al Jawf 001 (AJ 001) 29°44.57’N, 39°47.329’E Al Jawf, Saudi Arabia Found: 2009 May 7 Classification: Ordinary chondrite (H4-5) History: Mr. Jahn found the meteorite while he was working in Saudi Arabia. He brought the sample to the University of Tennessee in May 2013, where it was analyzed and identified as a meteorite. Physical characteristics: The stone is covered with black fusion crust and indentations. Petrography: The cut surface shows a coarse brecciated texture, with clasts ranging up to 4 cm. Abundant metal grains are visible. Clasts vary from relatively unshocked (S1) to impact melted. Geochemistry: The Fa and Fs values represent mean values of all the clasts.
Load more

Recommended publications
  • A New Sulfide Mineral (Mncr2s4) from the Social Circle IVA Iron Meteorite
    American Mineralogist, Volume 101, pages 1217–1221, 2016 Joegoldsteinite: A new sulfide mineral (MnCr2S4) from the Social Circle IVA iron meteorite Junko Isa1,*, Chi Ma2,*, and Alan E. Rubin1,3 1Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, California 90095, U.S.A. 2Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, U.S.A. 3Institute of Geophysics and Planetary Physics, University of California, Los Angeles, California 90095, U.S.A. Abstract Joegoldsteinite, a new sulfide mineral of end-member formula MnCr2S4, was discovered in the 2+ Social Circle IVA iron meteorite. It is a thiospinel, the Mn analog of daubréelite (Fe Cr2S4), and a new member of the linnaeite group. Tiny grains of joegoldsteinite were also identified in the Indarch EH4 enstatite chondrite. The chemical composition of the Social Circle sample determined by electron microprobe is (wt%) S 44.3, Cr 36.2, Mn 15.8, Fe 4.5, Ni 0.09, Cu 0.08, total 101.0, giving rise to an empirical formula of (Mn0.82Fe0.23)Cr1.99S3.95. The crystal structure, determined by electron backscattered diffraction, is aFd 3m spinel-type structure with a = 10.11 Å, V = 1033.4 Å3, and Z = 8. Keywords: Joegoldsteinite, MnCr2S4, new sulfide mineral, thiospinel, Social Circle IVA iron meteorite, Indarch EH4 enstatite chondrite Introduction new mineral by the International Mineralogical Association (IMA 2015-049) in August 2015. It was named in honor of Thiospinels have a general formula of AB2X4 where A is a divalent metal, B is a trivalent metal, and X is a –2 anion, Joseph (Joe) I.
    [Show full text]
  • V Xanes in Spinels As an Oxy-Barometer in Meteorites with Implications for Redox Variations in the Inner Solar System
    V XANES IN SPINELS AS AN OXY-BAROMETER IN METEORITES WITH IMPLICATIONS FOR REDOX VARIATIONS IN THE INNER SOLAR SYSTEM. K. Righter1, S. Sutton2, L. Danielson3, K. Pando4, L. Le3, and M. Newville2. 1NASA-JSC, 2101 NASA Pkwy., Houston, TX 77058 ([email protected]), 2GSECARS Uni- versity of Chicago, 9700 South Cass Avenue, Bldg. 434A, Argonne, IL 60439; 3ESCG, Jacobs Engineering, Houston, TX 77058; 4ESCG, Hamilton Sundstrand, Houston, TX 77058 Introduction: The variation of oxygen fugacity edge peak) depend on oxidation state and coordination within inner solar system materials spans a range of (e.g., [4,5]). In the present work, the intensity of the nearly 15 orders of magnitiude [1]. Igneous and meta- XANES pre-edge morphic rocks commonly contain a mineral assemblage that allows oxygen fugacity to be calculated or con- strained such as FeTi oxides, olivine-opx-spinel, or some other oxybarometer [2]. Some rocks, however, contain a limited mineral assemblage and do not pro- vide constraints on fO2 using mineral equilibria. Good examples of the latter are orthopyroxenites or dunites, such as diogenites, ALH 84001, chassignites, or bra- chinites. In fact it is no surprise that the fO2 of many of these achondrites is not well known, other than being "reduced" and below the metal saturation value. In or- der to bridge this gap in our understanding, we have initiated a study of V in chromites in achondrite. Be- cause the V pre-edge peak intensity and energy in chro- mites varies with fO2 (Fig. 1) [3], and this has been Figure 1: Correlation of V K pre-edge peak intensity calibrated over a large fO2 range, we can apply this with IW for spinels in the experiments of [3].
    [Show full text]
  • 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.
    [Show full text]
  • SPECTRAL CHARACTERIZATION of the ANCIENT SHERGOTTITES NORTHWEST AFRICA 7034 and 8159. KJ Orr1, LV Forman1, GK Benedix1
    Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6177.pdf SPECTRAL CHARACTERIZATION OF THE ANCIENT SHERGOTTITES NORTHWEST AFRICA 7034 AND 8159. K. J. Orr1, L. V. Forman1, G. K. Benedix1, M. J. Hackett2, V. E. Hamilton3, and A. R. Santos. 1Space Science and Technology Centre (SSTC), School of Earth and Planetary Sciences, Curtin University, Perth, Western Australia, Australia ([email protected]), 2School of Molecular and Life Sciences, Curtin University, Perth, Western Australia, Australia, 3Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302 USA. 4USRA, 7178 Columbia Gateway Dr., Columbia, MD 21046. Introduction: Thermal infrared (TIR) spectros- Ga), the oldest confirmed shergottites recovered so far copy is a powerful remote sensing tool used to unravel [5]. As the only shergottites of Early Amazonian to No- the surface compositions of a target body. This tech- achian in age, they provide an invaluable opportunity to nique has been widely used in space missions, because understanding Mars’ early history. of its ability to detect and determine modal mineralogy Methods: Both samples (~0.5g chips) were ac- of the surface geology. It has been instrumental in de- quired from UNM and were made into epoxy mounts. veloping our understanding of Mars, as the majority of NWA 8159 was analyzed with a Tescan Integrated Min- missions sent to Mars have included an infrared spec- eral Analyzer (TIMA) to determine modal mineral trometer. These spectrometers can operate either in the abundancies and produce high-resolution mineral maps. visible (VIS) to near-infrared (NIR) or in the mid-infra- NWA 8159 was also analyzed using EBSD to charac- red (MIR).
    [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]
  • 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.
    [Show full text]
  • Moon Minerals a Visual Guide
    Moon Minerals a visual guide A.G. Tindle and M. Anand Preliminaries Section 1 Preface Virtual microscope work at the Open University began in 1993 meteorites, Martian meteorites and most recently over 500 virtual and has culminated in the on-line collection of over 1000 microscopes of Apollo samples. samples available via the virtual microscope website (here). Early days were spent using LEGO robots to automate a rotating microscope stage thanks to the efforts of our colleague Peter Whalley (now deceased). This automation speeded up image capture and allowed us to take the thousands of photographs needed to make sizeable (Earth-based) virtual microscope collections. Virtual microscope methods are ideal for bringing rare and often unique samples to a wide audience so we were not surprised when 10 years ago we were approached by the UK Science and Technology Facilities Council who asked us to prepare a virtual collection of the 12 Moon rocks they loaned out to schools and universities. This would turn out to be one of many collections built using extra-terrestrial material. The major part of our extra-terrestrial work is web-based and we The authors - Mahesh Anand (left) and Andy Tindle (middle) with colleague have build collections of Europlanet meteorites, UK and Irish Peter Whalley (right). Thank you Peter for your pioneering contribution to the Virtual Microscope project. We could not have produced this book without your earlier efforts. 2 Moon Minerals is our latest output. We see it as a companion volume to Moon Rocks. Members of staff
    [Show full text]
  • Moore County Unbrecciated Cumulate Eucrite, 1.88Kg
    Moore County Unbrecciated Cumulate Eucrite, 1.88 kg Seen to fall Figure 1a: The Moore County eucrite (fusion crust on left), from the collection of the North Carolina Museum of Natural Sciences. Scale from top to bottom of sample is ~ 5 cm. Photo courtesy of Chris Tacker. Introduction: The Moore County meteorite (Figures 1a,b,c) fell at 5:00 PM on April 21, 1913, on the farm of George C. Graves, located approximately three miles east of Carthage, Moore County, North Carolina (79o23’W, 35o25’N) (Henderson and Davis, 1936). A loud “rumbling and zooming” noise “with no distinct explosions” was first observed within a five or six mile radius of the fall, followed by a sighting of a red hot ball with a 15-foot trail of blue-black smoke; the meteorite itself landed within a few feet of a farmer, in a nearly-vertical (but slightly SW-sloping) hole in a freshly-plowed field (Henderson and Davis, 1936). Only one stone was recovered (Figure 1b), weighing approximately 1.88 kg (4 lbs. 2 oz.), with maximum dimensions approximately 15 cm x 10.5 cm x 8 cm (6 in x 4 3/16 in x 3 3/16 in) (Henderson and Davis, 1936). This stone was divided between the US National Museum (Smithsonian) in Washington, D.C., and the North Carolina State Museum in Raleigh, now the North Carolina Museum of Natural Sciences (Henderson and Davis, 1936), where the main fractions of the stone are still kept (0.9 kg at the USNM and ~0.56 kg at the NC Museum: Grady, 2000; Tacker, pers.
    [Show full text]
  • The Investigated Rock Is One of the Gabbroic Bodies Which Crops out in the Surroundings of Lyngdal ( Extreme South of Norway)
    PYROXENE RELATIONS IN A HYPERITE NEAR LYNGDAL, NORWAY JOHAN J. LAVREAU Lavreau, J. J.: Pyroxene relations in a hyperite near Lyngdal, Norway. Norsk Geologisk Tidsskrift, Vol. 50, pp. 333-340. Oslo 1970. Pyroxenes from a hyperite body associated with Precambrian gneisses were studied optically, chemically, and by means of X-rays. Pyroxene relations show that crystallization takes place at a temperature higher than the inversion of pigeonite, and proceeds into the stability field of hypersthene. The composition and the mutual relations between the pyroxenes suggest a crystallization process for these minerals. Johan J. Lavreau, Laboratoire de Mineralogie et Petrologie, Universite Libre de Bruxelles, Brussels, Belgium. Introduction The investigated rock is one of the gabbroic bodies which crops out in the surroundings of Lyngdal ( extreme South of Norway). It Iies 3 km north of the town, northwest of Skoland lake, and is crossed by the E 18 road to Flekkefjord (Fig. 1). It is a well defined and homogeneous crescent-shaped unit, about 1500 m long and 500 m broad. The rock is medium grained (1-2 mm grain size), dark grey in colour, and has a gabbro-dioritic compo­ sition (Niggli 1923, p. 126). Some dioritic varieties were also recognized (Table 1). The country rock is a monzonitic phenoblastic gneiss foliated parallel to the elongation of the hyperite body. The contacts are seldom visible, for the area is covered by recent deposits except in its northern part, where the rock is unfortunately tectonized and strongly retrometa­ morphosed. Experimental techniques Plagioclase and pyroxenes were first studied with the aid of the universal stage.
    [Show full text]
  • Ron Hartman and the Lucerne Valley Meteorites by Robert Verish Ron Hartman and the Lucerne Valley Meteorites
    Meteorite Times Magazine Contents by Editor Featured Monthly Articles Accretion Desk by Martin Horejsi Jim's Fragments by Jim Tobin Meteorite Market Trends by Michael Blood Bob's Findings by Robert Verish IMCA Insights by The IMCA Team Micro Visions by John Kashuba Meteorite Calendar by Anne Black Meteorite of the Month by Editor Tektite of the Month by Editor Terms Of Use Materials contained in and linked to from this website do not necessarily reflect the views or opinions of The Meteorite Exchange, Inc., nor those of any person connected therewith. In no event shall The Meteorite Exchange, Inc. be responsible for, nor liable for, exposure to any such material in any form by any person or persons, whether written, graphic, audio or otherwise, presented on this or by any other website, web page or other cyber location linked to from this website. The Meteorite Exchange, Inc. does not endorse, edit nor hold any copyright interest in any material found on any website, web page or other cyber location linked to from this website. The Meteorite Exchange, Inc. shall not be held liable for any misinformation by any author, dealer and or seller. In no event will The Meteorite Exchange, Inc. be liable for any damages, including any loss of profits, lost savings, or any other commercial damage, including but not limited to special, consequential, or other damages arising out of this service. © Copyright 2002–2011 The Meteorite Exchange, Inc. All rights reserved. No reproduction of copyrighted material is allowed by any means without prior written permission of the copyright owner.
    [Show full text]
  • Pigeonite Basalt 2109 Grams
    12065 DRAFT Pigeonite Basalt 2109 grams Figure 1: Photo of 12065 showing numerous zap pits on rounded surface. Scale is in cm. NASA # S69-60591. Introduction Sample 12065 is a large rounded pigeonite basalt dated that near-surface olivine (Fo74) and some pyroxene at 3.16 ± 0.09 b.y. The outer surface is covered with settling could explain the variation in composition of micrometeorite pits on all sides (figure 1). some Apollo 12 basalts. Petrography Mineralogy 12065 is a variolitic basalt composed of pyroxene and Olivine: Olivine composition in 12065 ranges from olivine phenocrysts (figure 2) imbedded in a very fine Fo72-32 (Kushiro et al. 1971). matrix of feathery ilmenite, plagioclase and clinopyroxene (figure 3)(Reid 1971). Kushiro et al. Pyroxene: Hollister et al. (1971) and Kushiro et al. (1971) find that the fibrous pyroxene in 12065 is similar (1971) describe complex sector zoning of pyroxene to “quench pyroxenes” often found in quenching phenocrysts in 12065 (figure 4). Pigeonite cores are experiments. 12065 has a few percent void space. overgrown by subcalcic augite (Gay et al. 1971). Kushiro et al. report extreme Fe-enrichment in matrix Kushiro et al. (1971) used the bulk composition of pyroxene. Gay et al. report pyroxferroite with low Ca. 12065 to perform experiments leading to the conclusion Lunar Sample Compendium C Meyer 2005 Figure 2: Photomicrograph of thin section 12065 showing elongate pyroxene in variolitic groundmass. Scale is about 2 cm. NASA # S69-23378. Plagioclase: Plagioclase is An91 – An89 (Kushiro et al. 1971). Chemistry The chemical composition of 12065 has been reported Spinel: The Ti content of the Cr-spinel increases with by LSPET (1970), Maxwell et al.
    [Show full text]
  • 2713^7 Contents
    MINERALS OF WASHINGTON, D.C. AND VICINITY by Lawrence R. Bernstein U. S. Geo^r^'ce.l Survey OPEN F-'::. r;.".r'0.?;r cer.-..: 2713^7 CONTENTS Introduction 1 Scope of report 4 Mineral collecting 5 Acknowledgments 6 Introduction 6a ITT3 Aclj.il1 -> ! T^______.___~^. -"» _«_____«..«_»«__.. " " .._.«__._.._*_.__._.,_.._.-. _>-.-- -_>-->.-..-. Q Triassic deposits 31 Mineral localities 38 District of Columbia : 38 IMavtrlWlCfci JT XClilUl a Tirl ~ __ ___« - - -_ -»-i-___ .__- _ __- - ________________ m~m~m~ m~ m~ «M » M* **A^J ^ Anne Arundel County 43 Baltimore County 45 Howard County - 74 Montgomery County 88 Prince Georges County 120 Virginia . 129 Arlington County 129 Fairfax County 131 Fauquier County 139 Loudoun County 143 Prince William County 149 Diabase quarries of northern Virginia 155 CAPTIONS Illustrations Plate 1. Mineral localities of Washington, B.C., and vicinity. Plate 2. Generalized geologic map of Washington. D.C. and vicinity, Plate 3. Mineral deposits and generalized geology of the Triassic rocks near Washington, D.C. List of Figures Figure 1. Index map showing region covered in this report. Stfaded area is covered in most detail. Figure 2. Block diagram of the Washington, D.C. region showing physiographic provinces and major geographic and geologic features. ITfgure -3. Coastal Plain deposits of Washington, D.C. and vicinity. Figure 4. Generalized cross section of a typical complex pegmatite of the Washington, D.C. area. Figure 5. Rhythmically.layered gabbro of the Baltimore Gabbro Com­ plex at Ilchester, Maryland. Figure 6. Triassic diabase dike forming a ridge north of Route 7 near Dranesville, Virginia.
    [Show full text]