DOCSLIB.ORG

The Meteoritical Bulletin, No. 105

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Meteoritical Bulletin, No. 105 Meteoritics & Planetary Science 1 (2017) doi: 10.1111/maps.12944 The Meteoritical Bulletin, No. 105 Audrey BOUVIER1,Jerome^ GATTACCECA2, Jeffrey GROSSMAN3, and Knut METZLER4 1Department of Earth Sciences, University of Western Ontario, London, Ontario N6A 3K7, Canada 2CNRS, Centre de Recherche et d’Enseignement de Geosciences de l’Environnement, Aix-Marseille Universite, IRD, College de France, 13545, Aix En Provence, France 3NASA Headquarters, Washington, DC 20546, USA 4Institut fur€ Planetologie, Universitat€ Munster,€ Wilhelm-Klemm-Str. 10, 48149 Munster€ Germany Abstract–Meteoritical Bulletin 105 contains 2666 meteorites including 12 falls (Aouinet Legraa, Banma, Buritizal, Ejby, Kamargaon, Moshampa, Mount Blanco, Murrili, Osceola, Saricßicßek, Sidi Ali Ou Azza, Stubenberg), with 2244 ordinary chondrites, 142 HED achondrites, 116 carbonaceous chondrites, 37 Lunar meteorites, 20 enstatite chondrites, 20 iron meteorites, 20 ureilites, 19 Martian meteorites, 12 Rumuruti chondrites, 10 primitive achondrites, 9 mesosiderites, 5 angrites, 4 pallasites, 4 ungrouped achondrites, 2 ungrouped chondrites, 1 enstatite achondrite, and 1 relict meteorite, and with 1545 from Antarctica, 686 from Africa, 245 from Asia, 147 from South America, 22 from North America, 14 from Europe, 5 from Oceania, 1 from unknown origin. Note: 5 meteorites from Russia were counted as European. It also includes a list of approved new Dense Collection Areas and a nomenclature of the Aletai (IIIE-an) iron meteorites from Xinjiang, China. TABLE OF CONTENTS 1. Alphabetical text entries for non-Antarctic meteorites ................................................................................ 2 2. New Dense Collection Areas .....................................................................................................................249 3. Listing of institutes and collections ............................................................................................................249 4. Bibliography ...............................................................................................................................................249 5. Online supplement 1: Table of Data including Antarctic meteorites 6. Online supplement 2: Table of Corrections SUPPORTING INFORMATION information of this article as well as on the Meteoritical Bulletin Archive page at http://meteoriticalsociety.org/? Additional supporting information may be found in page_id=57. Information about the approved the online version of this article: meteorites can be obtained from the Meteoritical Data S1. A complete copy of entire Meteoritical Bulletin Database (MBD) available online at https:// Society Bulletin can be found in the supplementary www.lpi.usra.edu/meteor/. 1 © The Meteoritical Society, 2017. 1. Alphabetical text entries for non-Antarctic meteorites Abadla 30°56’13.04’’N, 2°42’56.40’’W Bechar, Algeria Find: 2015 Mar 15 Classification: HED achondrite (Eucrite, cumulate) History: Found by Mr. Abdelrahman about 15 km south of the village of Abadla, Algeria, on March 15, 2015. Purchased by Didi Moulay El Bechir in 2015. Physical characteristics: Single stone with black fusion crust. A saw cut reveals a mosaic of gray, coarse-grained, interlocking crystals. Petrography: (C. Agee, UNM) This cumulate rock consists of ~80% equilibrated, unzoned pyroxene, with no microscopically visible exsolution lamellae, and ~15% maskelynite. Most maskelynite domains are surrounded by pyroxene with radiating fractures suggesting shrinkage cracks. Accessory chromite, ilmenite, troilite, and iron oxide were observed. Geochemistry: (C. Agee and N. Muttik, UNM) Low-Ca pyroxene Fs39.1±1.3Wo2.9±1.5, Fe/Mn=30±1, n=15; augite Fs22.1±5.5Wo32.1±10.0, Fe/Mn=28±3, n=5; plagioclase An92.6±0.4, n=10. Classification: Cumulate eucrite Specimens: 21.12 g including a probe mount on deposit at UNM, Didi Moulay El Bechir holds the main mass. Abarkouh 001 31°18.26’N, 53°10.30’E Fars, Iran Find: 2014 May 18 Classification: Ordinary chondrite (L5) History: Meteorites were found during a systematic search conducted by the AsemanSang group. A sample was sent to H. Pourkhorsandi in January 2016. Physical characteristics: Samples are partially covered by a dark-brown crust. Cut surface shows a light-brown interior. Petrography: Recrystallized chondritic texture. FeNi metal and troilite are well separated. Some weathering veins can be seen. Troilite shows limited weathering. Chromite-plagioclase assemblages are present. Classification: L5 based on petrography and magnetic susceptibility. Specimens: Type specimen 27 g and a polished section at CEREGE. 17 g and a thin section at New England Meteoritical Services (NEMS). Al Haggounia 004 27°6’24’’N, 12°1’36’’W Saguia el Hamra, Western Sahara Find: 15 Jan 2015 Classification: Carbonaceous chondrite (CK3) History: Four brownish fragments were found by Mr. Zaid Balli at Ouad Ouinaght and subsequently purchased by Marcin Cimala. Physical characteristics: The meteorite shows a strongly altered brownish-orange sawn surface. Petrography: The meteorite is composed of separated and clearly defined chondrules set into abundant olivine-rich matrix. Few chondrules contain compositionally unequilibrated olivine and less abundant low-Ca pyroxene. Throughout the matrix olivine is equilibrated. Cr-bearing magnetite and intermediate plagioclase are abundant in the matrix; accessories include Ca- pyroxene, pyrrhotite and troilite. Geochemistry: Equilibrated matrix olivine: Fa29.4±0.3, n=16; unequilibrated olivine: Fa12.8±10.2 (Fa2.2-29.1, n=15); low-Ca pyroxene: Fs23.0±1.6Wo0.6±0.1 (Fs21.1-24.7Wo0.4-0.8, n=6); Ca-pyroxene: Fs18.3Wo49.2 (N=2); C2O3 in magnetite: 3.8 wt% (N=4) Alatage Mountain 042 (AM 042) 41°41’19.8"N, 92°57’10.4"E Xinjiang, China Find: 1 May 2013 Classification: Ordinary chondrite (L5) History: An expedition found 42 meteorites between 30 April and 1 May 2013 in a 2.7 × 1.4 km area 80 km east of Alatage Mountain. The expedition included Bingkui Miao, Yangting Lin, Shijie Li, Deqiu Dai, Wenjie Shen, Sen Hu, Lei Kesi, Peng Wang, and Zhipeng Xia. Physical characteristics: Total mass: 403.8 g (only 1 piece) no fusion crust, gray surface Petrography: The meteorite shows a homogeneous lithology. The sizes of minerals are mostly <100 μm. Mosaic extinction of olivine is common. More than 50% of metal and sulfide is oxidized. Geochemistry: Minerals are uniform. Olivine: Fa22.2±0.7 (n=9); low-Ca pyroxene: Fs19.1±2.2Wo4.7±1.9 (n=9) Classification: Ordinary chondrite (L5); S5; W2. Specimens: 100 g sample and one thin section are deposited in GUT. Nomenclature of the Aletai (IIIE-an) iron meteorites from Xinjiang, China Chemical and petrographic analyses of multiple iron meteorite masses in the northern part of Xinjiang Uyghur Autonomous Region, China, indicate pairing of these masses with the Armanty (IIIE) iron. All of these iron meteorites, as well any paired material that may be discovered in the future, will henceforth carry the official name “Aletai,” the name of a local county. The names “Armanty,” “Xinjiang (b),” and “Xinjiang 008” (a provisional name) are now abolished, and become synonyms for Aletai. In a previous action (MetBull 95), the name “Ulasitai” was abolished, and made a synonym for Armanty; “Ulasitai” will now become a synonym for Aletai. This entry also corrects previously published coordinates for the 28 tonne Armanty mass, announces several new masses, and presents compositional data by J.T. Wasson, UCLA, for five of the paired masses. The masses form a NW-SE array, spanning approximately 425 km across China and a sliver of Mongolia (although no masses have been reported from Mongolia). The new nomenclatural system for these irons is analogous to the grouping, some decades ago, of previously named IIAB irons under the name “North Chile.” When referring generally to the irons, authors should use the names “Aletai” and “North Chile.” When referring to a specific mass, authors should identify it as, for example, the "Armanty mass of Aletai" or the "Filomena mass of North Chile." The list of recommended mass names for Aletai appears in the table below. The coordinates listed for this entry correspond to the corrected location at which the Armanty mass was discovered. Discovery of the Wuxilike mass of Aletai: History: A large iron was found by a local farmer in a valley in a mountainous area of Aletai County. It was surrounded by rocks and half buried. A small specimen was taken for analysis. Heavy machinery was used to move the meteorite from the valley to the discoverer’s home. Physical characteristics: The kamacite bandwidth is 0.89±0.41 mm. Petrography: The major phases of the meteorite are kamacite, taenite, and plessite. Minor phases include schreibersite, daubréelite, troilite, and haxonite. Discovery of the Akebulake mass of Aletai: An account of the discovery of this large iron mass in a remote mountainous region was published by Beatty (2011) based on a trip there by Ayisha in June 2011. It has an irregular surface with partial regmaglypts but has been severely affected by terrestrial weathering. The iron is dark-brown; it was partly covered by a granite slab on the side of a mountain. Its exterior was marked by several scrawls of graffiti and cuts. Aletai City officials worried that the meteorite would be further damaged they built a road and moved the Akebulake mass to the Aletai city hall in 2011. Table 1. Known masses of Aletai. Analyses by J. T. Wasson, UCLA, See MetBull 104 for an analysis of Xinjiang (b). Aletai is an anomalous IIIE. It has
Load more

Recommended publications
  • Eat and Die: the Last Meal of Sacrificed Chimú Camelids At
    Eat and Die: The Last Meal of Sacrificed Chimú Camelids at Huanchaquito-Las Llamas, Peru, as Revealed by Starch Grain Analysis Clarissa Cagnato , Nicolas Goepfert, Michelle Elliott, Gabriel Prieto, John Verano, and Elise Dufour This article reconstructs the final diet of sacrificed domestic camelids from Huanchaquito-Las Llamas to understand whether feeding was part of the ritual practice. The site is situated on the northern coast of Peru and is dated to the fifteenth century AD (Late Intermediate period; LIP). It was used by the Chimús to kill and bury a large number of camelids, mostly juveniles. We reconstructed the final meal of 11 of the sacrificed individuals by analyzing starch grains derived from the associated gut con- tents and feces. The starch grains were well preserved and allowed for the determination of five plant taxa. The comparison with previously published and new stable isotope analyses, which provide insights into long-term diet, indicates that the Chi- mús managed their herds by providing maize as fodder and allowing them to graze on natural pasture; yet they reserved special treatment for sacrificial animals, probably bringing them together a few hours or days before the sacrificial act. We show for the first time the consumption of unusual food products, which included manioc, chili peppers, and beans, as well as cooked foods. Our study provides unique information on Chimú camelid ritual and herding practices. Keywords: ritual diet, archaeobotany, stable isotope analysis, Late Intermediate period El presente artículo aborda la reconstrucción de la dieta ingerida por camélidos domesticados antes de ser sacrificados y enterrados en el sitio arqueológico Huanchaquito-Las Llamas, situado en la costa norte de Perú y data del siglo XV de nuestra era (periodo Intermedio Tardío).
    [Show full text]
  • Olivine and Pyroxene from the Mantle of Asteroid 4 Vesta ∗ Nicole G
    Earth and Planetary Science Letters 418 (2015) 126–135 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Olivine and pyroxene from the mantle of asteroid 4 Vesta ∗ Nicole G. Lunning a, , Harry Y. McSween Jr. a,1, Travis J. Tenner b,2, Noriko T. Kita b,3, Robert J. Bodnar c,4 a Department of Earth and Planetary Sciences and Planetary Geosciences Institute, University of Tennessee, Knoxville, TN 37996, USA b Department of Geosciences, University of Wisconsin, Madison, WI 53706, USA c Department of Geosciences, Virginia Tech, Blacksburg, VA 24061, USA a r t i c l e i n f o a b s t r a c t Article history: A number of meteorites contain evidence that rocky bodies formed and differentiated early in our solar Received 25 September 2014 system’s history, and similar bodies likely contributed material to form the planets. These differentiated Received in revised form 25 February 2015 rocky bodies are expected to have mantles dominated by Mg-rich olivine, but direct evidence for such Accepted 25 February 2015 mantles beyond our own planet has been elusive. Here, we identify olivine fragments (Mg# = 80–92) in Available online 17 March 2015 howardite meteorites. These Mg-rich olivine fragments do not correspond to an established lithology Editor: T. Mather in the howardite–eucrite–diogenite (HED) meteorites, which are thought to be from the asteroid 4 Keywords: Vesta; their occurrence in howardite breccias, combined with diagnostic oxygen three-isotope signatures planetary formation and minor element chemistry, indicates they are vestan.
    [Show full text]
  • 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]
  • Assessment of the Mesosiderite-Diogenite Connection and an Impact Model for the Genesis of Mesosiderites
    45th Lunar and Planetary Science Conference (2014) 2554.pdf ASSESSMENT OF THE MESOSIDERITE-DIOGENITE CONNECTION AND AN IMPACT MODEL FOR THE GENESIS OF MESOSIDERITES. T. E. Bunch1,3, A. J. Irving2,3, P. H. Schultz4, J. H. Wittke1, S. M. Ku- ehner2, J. I. Goldstein5 and P. P. Sipiera3,6 1Dept. of Geology, SESES, Northern Arizona University, Flagstaff, AZ 86011 ([email protected]), 2Dept. of Earth & Space Sciences, University of Washington, Seattle, WA, 3Planetary Studies Foundation, Galena, IL, 4Dept. of Geological Sciences, Brown University, Providence, RI, 5Dept. of Geolo- gy, University of Massachusetts, Amherts, MA, 6Field Museum of Natural History, Chicago, IL. Introduction: Among well-recognized meteorite 34) is the most abundant silicate mineral and in some classes, the mesosiderites are perhaps the most com- clasts contains inclusions of FeS, tetrataenite, merrillite plex and petrogenetically least understood. Previous and silica. Three of the ten norite clasts contain a few workers have contributed important information about tiny grains of olivine (Fa24-32). A single, fine-grained “classic” falls and Antarctic finds, and have proposed breccia clast was found in NWA 5312 (see Figure 2). several different models for mesosiderite genesis [1]. Unlike the case of pallasites, the co-occurrence of met- al and silicates (predominantly orthopyroxene and cal- cic plagioclase) in mesosiderites is inconsistent with a single-stage “igneous” history, and instead seems to demand admixture of at least two separate compo- nents. Here we review the models in light of detailed ex- amination of multiple specimens from a very large mesosiderite strewnfield in Northwest Africa. Many specimens (totaling at least 80 kilograms) from this area (probably in Algeria) have been classified sepa- rately by us and others; however, in most cases the Figure 1.
    [Show full text]
  • TUPELO, a NEW EL6 ENSTATITE CHONDRITE. DR Dunlap1
    44th Lunar and Planetary Science Conference (2013) 2088.pdf TUPELO, A NEW EL6 ENSTATITE CHONDRITE. D. R. Dunlap1 ([email protected]), M. L. Pewitt1 ([email protected]), H. Y. McSween1, Raymond Doherty2, and L. A. Taylor1, 1Planetary Geoscience Institute, De- partment of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, 37996, USA, 24441 W Main Street, Tupelo, MS 38801, USA. Introduction: Enstatite chondrites are the rarest phosphides, and metal. Modal analyses of the two and most reduced chondrite clan [1]. E-chondrites are analyzed sections are given in Table 1. The subdivided into two groups, EL and EH, based on kamcite/silicate ratios of both sections are consistent modal iron-metal abundances. E-chondrites are charac- with EL chondrites. terized by the presence of nearly pure enstatite and silicon-bearing metal, with ferroan-alabandite in EL and niningerite in EH. Additionally, elements that are typically lithophilic in most meteorite groups (e.g., Mn, Mg, Ca, Na, K) can behave like chalcophile ele- ments in the E-chondrites due to the extremely reduc- ing conditions, forming a variety of accessory phases. Table 1. Modal analyses of Tupelo after [3]. * include graphite, Metamorphic characteristics used to define petrologic schreibersite, and all other non-sulfide, non-silicate minerals present. types [2] do not apply well to E-chondrites; therefore, **Troilite also includes alabandite and daubreelite. mineralogic types are utilized to specify metamorphic grade [3]. The silicates are nearly FeO-free enstatite (En98) The 280g Tupelo meteorite was found in 2012 by and sodic plagioclase feldspar (Ab77.7Or4.8). This feld- Maura O’Connell and Raymond Doherty, in a field in spar composition is consistent with composition re- Mississippi while looking for Indian artifacts.
    [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]
  • 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]
  • A Multielement Isotopic Study of Refractory FUN and F Cais: 2 Mass-Dependent and Mass-Independent Isotope Effects 3 Levke Kööp1,2,3,*, Daisuke Nakashima4,5, Philipp R
    1 A multielement isotopic study of refractory FUN and F CAIs: 2 Mass-dependent and mass-independent isotope effects 3 Levke Kööp1,2,3,*, Daisuke Nakashima4,5, Philipp R. Heck1,2,3, Noriko T. Kita4, Travis J. Ten- 4 ner4,6, Alexander N. Krot7, Kazuhide Nagashima7, Changkun Park7,8, Andrew M. Davis1,2,3,9 5 1Department of the Geophysical Sciences, The University of Chicago, Chicago, IL 60637, 6 USA ([email protected]) 7 2Chicago Center for Cosmochemistry, The University of Chicago, Chicago, IL 60637, USA 8 3Robert A. Pritzker Center for Meteoritics and Polar Studies, Field Museum of Natural His- 9 tory, Chicago, IL, USA 10 4Department of Geoscience, University of Wisconsin, Madison, WI 53706, USA 11 5Division of Earth and Planetary Material Sciences, Faculty of Science, Tohoku University, 12 Aoba, Sendai, Miyagi 980-8578 Japan 13 6 Chemistry Division, Nuclear and Radiochemistry, Los Alamos National Laboratory, 14 MSJ514, Los Alamos, NM 87545, USA 15 7Hawai‘i Institute of Geophysics and Planetology, School of Ocean and Earth Science and 16 Technology, University of Hawai‘i at M!noa, Honolulu, HI 17 8Korea Polar Research Institute, Incheon 21990, Korea 18 9Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA. 19 20 *E-mail address of the corresponding author: [email protected] 21 ABSTRACT 22 Calcium-aluminum-rich inclusions (CAIs) are the oldest dated objects that formed inside the 23 Solar System. Among these are rare, enigmatic objects with large mass-dependent fractionation 24 effects (F CAIs), which sometimes also have large nucleosynthetic anomalies and a low initial 25 abundance of the short-lived radionuclide 26Al (FUN CAIs).
    [Show full text]
  • Meteorite Dunite Breccia Mil 03443: a Probable Crustal Cumulate Closely Related to Diogenites from the Hed Parent Asteroid
    METEORITE DUNITE BRECCIA MIL 03443: A PROBABLE CRUSTAL CUMULATE CLOSELY RELATED TO DIOGENITES FROM THE HED PARENT ASTEROID. David W Mittlefehldt, Astromateri- als Research Office, NASA/Johnson Space Center, Houston, Texas, USA, ([email protected]). Introduction: There are numerous types of differ- Metal is very rare, and occurs as grains a few microns entiated meteorites, but most represent either the crusts in size associated with troilite. or cores of their parent asteroids. Ureilites, olivine- pyroxene-graphite rocks, are exceptions; they are man- tle restites [1]. Dunite is expected to be a common mantle lithology in differentiated asteroids. In particu- lar, models of the eucrite parent asteroid contain large volumes of dunite mantle [2-4]. Yet dunites are very rare among meteorites, and none are known associated with the howardite, eucrite, diogenite (HED) suite. Spectroscopic measurements of 4 Vesta, the probable HED parent asteroid, show one region with an olivine signature [5] although the surface is dominated by ba- saltic and orthopyroxenitic material equated with eucrites and diogenites [6]. One might expect that a small number of dunitic or olivine-rich meteorites might be delivered along with the HED suite. The 46 gram meteoritic dunite MIL 03443 (Fig. 1) Figure 2. BSE image of MIL 03443 showing its gen- was recovered from the Miller Range ice field of Ant- eral fragmental breccia texture, and primary texture arctica. This meteorite was tentatively classified as a between olivine, orthopyroxene and chromite. mesosiderite because large, dunitic clasts are found in this type of meteorite, but it was noted that MIL 03443 could represent a dunite sample of the HED suite [7].
    [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]
  • Olivine-Dominated Asteroids and Meteorites: Distinguishing Nebular and Igneous Histories
    Meteoritics & Planetary Science 42, Nr 2, 155–170 (2007) Abstract available online at http://meteoritics.org Olivine-dominated asteroids and meteorites: Distinguishing nebular and igneous histories Jessica M. SUNSHINE1*, Schelte J. BUS2, Catherine M. CORRIGAN3, Timothy J. MCCOY4, and Thomas H. BURBINE5 1Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA 2University of Hawai‘i, Institute for Astronomy, Hilo, Hawai‘i 96720, USA 3Johns Hopkins University, Applied Physics Laboratory, Laurel, Maryland 20723–6099, USA 4Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, D.C. 20560–0119, USA 5Department of Astronomy, Mount Holyoke College, South Hadley, Massachusetts 01075, USA *Corresponding author. E-mail: [email protected] (Received 14 February 2006; revision accepted 19 November 2006) Abstract–Melting models indicate that the composition and abundance of olivine systematically co-vary and are therefore excellent petrologic indicators. However, heliocentric distance, and thus surface temperature, has a significant effect on the spectra of olivine-rich asteroids. We show that composition and temperature complexly interact spectrally, and must be simultaneously taken into account in order to infer olivine composition accurately. We find that most (7/9) of the olivine- dominated asteroids are magnesian and thus likely sampled mantles differentiated from ordinary chondrite sources (e.g., pallasites). However, two other olivine-rich asteroids (289 Nenetta and 246 Asporina) are found to be more ferroan. Melting models show that partial melting cannot produce olivine-rich residues that are more ferroan than the chondrite precursor from which they formed. Thus, even moderately ferroan olivine must have non-ordinary chondrite origins, and therefore likely originate from oxidized R chondrites or melts thereof, which reflect variations in nebular composition within the asteroid belt.
    [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]