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The Meteoritical Bulletin, No. 102 1 2 3 4 5 ALEX RUZICKA , JEFFREY GROSSMAN , AUDREY BOUVIER , CHRISTOPHER D.K

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The Meteoritical Bulletin, No. 102 1 2 3 4 5 ALEX RUZICKA , JEFFREY GROSSMAN , AUDREY BOUVIER , CHRISTOPHER D.K The Meteoritical Bulletin, No. 102 1 2 3 4 5 ALEX RUZICKA , JEFFREY GROSSMAN , AUDREY BOUVIER , CHRISTOPHER D.K. HERD and CARL B. AGEE 1Cascadia Meteorite Laboratory, Department of Geology, Portland State University, Portland, Oregon, 97207-0751, USA 2NASA Headquarters, Mail Stop 3E46, 300 E Street, SW, Washington, D.C., 20546, USA 3Western University, Department of Earth Sciences, London, Ontario, N6A B57, Canada 4University of Alberta, Department of Earth and Atmospheric Sciences, Edmonton, Alberta, T6G 2E3, Canada 5Institute of Meteoritics, Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, New Mexico, 87131-0001, USA Abstract: Meteoritical Bulletin 102 contains 3141 meteorites including 12 falls (Boumdeid (2003), Boumdeid (2011), Braunschweig, Chelyabinsk, Dongyang, Draveil, Heyetang, Indian Butte, Katol, Ladkee, Ouadangou, Xining), with 2611 Ordinary chondrites, 264 HED achondrites, 124 Carbonaceous chondrites, 30 Ureilites, 20 Martian meteorites, 16 Primitive achondrites, 16 Rumuruti chondrites, 15 Mesosiderites, 12 Iron meteorites, 10 Lunar meteorites, 9 Enstatite chondrites, 4 Enstatite achondrites, 4 Pallasites, 4 Ungrouped achondrites, and 2 Angrites, and with 1708 from Antarctica, 956 from Africa, 294 from South America, 126 from Asia, 47 from North America, 6 from Europe (including Russia), and 4 from Oceania. Information about approved meteorites can be obtained from the Meteoritical Bulletin Database (MBD) available on line at http://www.lpi.usra.edu/meteor/ . A complete copy of this Bulletin (248 pages) is available electronically. Table of Contents 1. Information on dense collection areas.................……………………………………………..F2 2. Alphabetical text entries for non-Antarctic meteorites ..…………….…………………….…F2 3. Bibliography ……………………..……………………………………………………….. F172 4. Alphabetical listing of all meteorites ..………..…………………………………….……...F172 5. Corrected entries ………………..…………………………………………..……………...F244 6. Listing of institutes and collections …..……………………………………..……………..F244 7. Acknowledgments …………………..…………………………………………..…………F248 The Meteoritical Bulletin was published on 19 AUG 2015 without the complete listing, it has been corrected. 1. Information on dense collection areas Dense collection areas (DCAs) are specific regions on the surface of the Earth where place names are sparse and where numerous meteorite recoveries are made (Section 3.3c of the Guidelines on Meteorite Nomenclature). Naming of meteorites found in these areas is done using a generic prefix and a series of numbers; meteorites found in an area corresponding to an existing DCA are given a name that includes the next number in the sequence. The assignment of the next number in the sequence is done by the online submission system, i.e., at the time of submission of the meteorite classification file. Prefixes and their abbreviations are adjudicated and approved by the Nomenclature Committee to ensure that they convey geographic information and to avoid duplication of abbreviations. The committee maintains a complete list of approved DCAs, including abbreviations and maps in KML format (which can be read using Google Earth). Most new DCAs are defined by submitters of meteorites found in areas requiring the establishment of a DCA. In order to streamline the process, the Nomenclature Committee created a DCA Coordinator position (held by Knut Metzler, 2013-present). In 2015 a DCA subcommittee was struck in order to establish DCAs in Morocco and surrounding areas following a change to the Guidelines that eliminates special rules for meteorites found in these areas. New DCA proposals should include all the information required for the Nomenclature Committee to adjudicate the request (maps, imagery and/or written descriptions outlining the geographic extent, etc.); however, the most frequently used, simplest method is to outline an area using Google Earth and submit the KML file to the DCA Coordinator (email: [email protected]). 2. Alphabetical text entries for non-Antarctic meteorites Agoudal 31°59.074’N, 5°30.917’W Centre-South, Morocco Found: 2000 Classification: Iron meteorite (IIAB) History: (H. Chennaoui Aoudjehane, M. Aboulahris, FSAC) Two small pieces of iron were collected in 2000 in the Agoudal area, High Atlas Mountains, Morocco, and sold to tourists. In September 2011, one piece was sold to a dealer in Errich, who recognized it as an iron meteorite. During the last months of 2012, systematic searching by meteorite hunters with metal detectors resulted in the discovery of a large number of meteorites, mostly small. Many pieces were collected on the surface or buried a few cm deep. The largest piece recovered was 60 kg, buried ~50 cm below the surface. On 9 February 2013, H. Chennaoui Aoudjehane, M. Aoudjehane and M. Aboulahris collected 200 g of specimens; the listed coordinates are those of the largest piece they recovered. The strewnfield is not yet clearly defined. Physical characteristics: Total mass is >100 kg. Hundreds of small pieces (1-100 g), many 100-1000 g, and a few pieces >1 kg, have been recovered. The majority of collected material occurs as 2-5 cm, irregularly shaped shrapnel pieces. Most pieces have a thin weathering rind. Some smaller bullet-shaped (~cm-sized) fragments are rounded, showing well-developed fusion crust. Petrography: (L. Garvie, ASU) Decimeter-sized pieces show a coarse pattern of irregular, interlocking kamacite grains; some grains with sub-boundaries. Widmanstätten pattern not evident in the small sections studied. Grain boundaries commonly curved. Etched pieces range from shiny with well- developed Neumann bands, to pieces with a matte appearance, typical of the hatched ε-structure. The shock-hatched regions show incipient recrystallization, with secondary growth of irregularly-shaped (to 1 mm) kamacite. No plessite observed. Schreibersite abundant occurring as cm-sized skeletal crystals at the centers of kamacite crystals, as rhabdites, and as a grain boundary precipitate. Rhabdites locally numerous 2 as sharp, 10-25 μm faceted prisms. Scattered troilite nodules, to 1 cm. Troilite not surrounded by schreibersite, but instead large skeletal schreibersite is situated a few mm away. Heat-affected zone visible on some stones. Several of the smaller pieces, and especially the rounded bullet-shaped stones, have fusion crust and heated-affected zone of varying thickness; some completely recrystallized. Geochemistry: (C. Herd and G. Chen, UAb): ICP-MS data, Ni 5.5 wt%, Co 4.1 mg/g, Ga 58 μg/g, Ir < 0.04 μg/g and Au ~ 1 μg/g. Classification: Iron, IIAB. Structurally similar to Ainsworth. Specimens: Type specimens include 2406 g, ASU; 17.5 g, UAb; 200 g, FSAC Other names: This meteorite has been sold and traded under the name "Imilchil" Ariah Park 34°18.92’S, 147°14.47’E New South Wales, Australia Found: 1932 Classification: Iron meteorite (IIIAB) History: The meteorite was found in a dry creek bed by James Richard Keys in 1932, while he was walking with hunting dogs. It has been in possession of the Keys family since that date. It is named after a breached dam near Ariah Park, County Bland, Parish Mandamah, 44 km from S of West Wyalong, 35 km WNW of Temora, New South Wales. Petrography: (A. Bevan, WAM). The meteorite is an octahedrite containing kamacite, taenite and large plessite fields. Kamacite bandwidth could not be determined accurately due to the small section examined. Kamacite is shock-hardened (ε-kamacite) and contains deformation bands. Kamacite contains abundant, small schreibersite crystals (rhabdites), platelets of carlsbergite, and rare daubréelite. Terrestrial oxidation has penetrated deeply along grain boundaries. Geochemistry: (J.T. Wasson, UCLA): Ni = 77.4, Co = 4.97 (both mg/g), Cu = 167, Ga = 18.4, As = 3.86, Ir = 9.14, Au = 0.575 (all μg/g), W = 1.21 ng/g. Similar to Boxhole. Classification: Iron, Group IIIAB medium to coarse octahedrite Specimens: Type specimen, 24.8 g, AMSA. Main mass with the finder’s son, Patrick James Keys. Biduna Blowhole 004 31°1’58.0"S, 131°17’7.9"E South Australia, Australia Found: 6 Apr 2011 Classification: Ordinary chondrite (H5) History: Single piece found by A. Tomkins on the Nullarbor Plain. Physical characteristics: Unusually shaped 8 × 2.5 × 2 cm stone, dense, rounded edges, lacking fusion crust. Petrography: (E. Mare, Monash) Sample contains few well-defined chondrules (largest is 2 mm) and recrystallized and rusted matrix. Chondrule types include CC, RP, POP, PP, BO. Fe-Ni metal grains (5%) are 250 μm on average. Troilite grains (3%) are 50-100 μm on average. Both metal and troilite have been partly replaced by oxides, however only to a limited extent, with ~5% oxides in this meteorite. Olivine grains show slightly undulose extinction and occasionally planar fractures. There is evidence of melt pockets where troilite and metal have flowed around silicate grains. Geochemistry: (E. Mare, Monash) Microprobe analyses show that olivine and pyroxene compositions are uniform: olivine Fa19.4-20.0, mean=Fa19.6, std=0.3, n=4; Low-Ca pyroxene Fs17.4-18.0, mean=Fs17.5, std=0.3, n=4. Classification: Ordinary chondrite (H5, S3, W2) Bou Kra 004 26.707°N, 12.759°W Saguia el Hamra, Western Sahara Found: 2010 Sep 25 Classification: HED achondrite (Eucrite, monomict) 3 History: Found by Pjotr Muromov and Svend Buhl on September 25, 2010, on the G’idat Amwizirat plateau in Western Sahara (substrate is fine-grained limestone and chert desert pavement). Physical characteristics: Two fresh, larger fragments (130.4 g and 93.80 g) coated by black fusion crust (and in turn by clusters of the fruticose lichen Ramalina maciformis), plus many small fragments weighing 17.0 g (>5 mm) and 31.5 g (<5 mm) total. All fragments were found within a 3.5 m radius, and fit together to form a heart-shaped and completely fusion-crusted mass. Petrography: (A. Irving and S. Kuehner, UWS): Ophitic assemblage of exsolved pigeonite and calcic plagioclase with accessory silica polymorph, ilmenite, troilite, Ti-chromite and rare zircon. Pyroxenes contain dusty zones of microscopic troilite inclusions. Geochemistry: Low-Ca pyroxene Fs58.8Wo5.6 (FeO/MnO = 29.8-30.7), high-Ca pyroxene Fs28.3-28.5Wo42.0- 41.9 (FeO/MnO = 33.1-33.9).
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