Meteoritics & Planetary Science, Volume 43, Number 5 (2008)http://hdl.handle.net/10150/6412372024-03-29T06:58:11Z2024-03-29T06:58:11ZBook Review: Oxygen in the Solar System, Glenn MacPherson (Ed.)Lyon, Ianhttp://hdl.handle.net/10150/6564362021-02-13T01:12:40Z2008-01-01T00:00:00ZBook Review: Oxygen in the Solar System, Glenn MacPherson (Ed.)
Lyon, Ian
Book Review: Oxygen in the Solar System, Glenn MacPherson (Ed.). Reviews in Mineralogy and Geochemistry, vol. 68. Washington, D.C.: Mineralogical Society of America (2008).
2008-01-01T00:00:00ZBook Review: Meteorites and the Early Solar System II, Dante S. Lauretta, Harry Y. McSween, Jr (Eds.)Trigo-Rodríguez, Josep M.http://hdl.handle.net/10150/6564372021-02-13T01:12:46Z2008-01-01T00:00:00ZBook Review: Meteorites and the Early Solar System II, Dante S. Lauretta, Harry Y. McSween, Jr (Eds.)
Trigo-Rodríguez, Josep M.
Book Review: Meteorites and the Early Solar System II, Dante S. Lauretta, Harry Y. McSween, Jr (Eds.). Tucson, Arizona: The University of Arizona Press (2006).
2008-01-01T00:00:00ZMagnetic classification of stony meteorites: 2. Non-ordinary chondritesRochette, PierreGattacceca, JérômeBonal, LydieBourot-Denise, MichèleChevrier, VincentClerc, Jean-PierreConsolmagno, GuyFolco, LuigiGounelle, MatthieuKohout, TomasPesonen, LauriQuirico, EricSagnotti, LeonardoSkripnik, Annahttp://hdl.handle.net/10150/6564342021-02-13T01:12:25Z2008-01-01T00:00:00ZMagnetic classification of stony meteorites: 2. Non-ordinary chondrites
Rochette, Pierre; Gattacceca, Jérôme; Bonal, Lydie; Bourot-Denise, Michèle; Chevrier, Vincent; Clerc, Jean-Pierre; Consolmagno, Guy; Folco, Luigi; Gounelle, Matthieu; Kohout, Tomas; Pesonen, Lauri; Quirico, Eric; Sagnotti, Leonardo; Skripnik, Anna
A database of magnetic susceptibility (Chi) measurements on different non-ordinary chondrites (C, E, R, and ungrouped) populations is presented and compared to our previous similar work on ordinary chondrites. It provides an exhaustive study of the amount of iron-nickel magnetic phases (essentially metal and magnetite) in these meteorites. In contrast with all the other classes, CM and C show a wide range of magnetic material content, with a two orders of magnitude variation of Chi. Whether this is due to primary parent body differences, metamorphism or alteration, remains unclear. C3-4 and C2 yield similar Chi values to the ones shown by CK and CM, respectively. By order of increasing Chi, the classes with well-grouped Chi are: R << CO < CK is approximately equal to CI < Kak < CR < E is approximately equal to CH < CB. Based on magnetism, EH and EL classes have indistinguishable metal content. Outliers that we suggest may need to have their classifications reconsidered are Acfer 202 (CO), Elephant Moraine (EET) 96026 (C4-5), Meteorite Hills (MET) 01149, and Northwest Africa (NWA) 521 (CK), Asuka (A(+)-88198, LaPaz Icefield (LAP) 031156, and Sahara 98248 (R). Chi values can also be used to define affinities of ungrouped chondrites, and propose pairing, particularly in the case of CM and CV meteorites.
2008-01-01T00:00:00ZThe Isheyevo meteorite: Mineralogy, petrology, bulk chemistry, oxygen, nitrogen, carbon isotopic compositions, and 40Ar-39Ar agesIvanova, Marina A.Kononkova, Natalia N.Krot, Alexander N.Greenwood, Richard C.Franchi, Ian A.Verchovsky, Alexander B.Trieloff, MarioKorochantseva, Ekaterina V.Brandstatter, Franzhttp://hdl.handle.net/10150/6564322021-02-13T01:11:53Z2008-01-01T00:00:00ZThe Isheyevo meteorite: Mineralogy, petrology, bulk chemistry, oxygen, nitrogen, carbon isotopic compositions, and 40Ar-39Ar ages
Ivanova, Marina A.; Kononkova, Natalia N.; Krot, Alexander N.; Greenwood, Richard C.; Franchi, Ian A.; Verchovsky, Alexander B.; Trieloff, Mario; Korochantseva, Ekaterina V.; Brandstatter, Franz
Isheyevo is a metal-rich carbonaceous chondrite that contains several lithologies with different abundances of Fe,Ni metal (7-90 vol%). The metal-rich lithologies with 5060 vol% of Fe,Ni metal are dominant. The metal-rich and metal-poor lithologies are most similar to the CBb and CH carbonaceous chondrites, respectively, providing a potential link between these chondrite groups. All lithologies experienced shock metamorphism of shock stage S4. All consist of similar componentsFe,Ni metal, chondrules, refractory inclusions (Ca, Al-rich inclusions [CAIs] and amoeboid olivine aggregates [AOAs]), and heavily hydrated lithic clastsbut show differences in their modal abundances, chondrule sizes, and proportions of porphyritic versus non-porphyritic chondrules. Bulk chemical and oxygen isotopic compositions are in the range of CH and CB chondrites. Bulk nitrogen isotopic composition is highly enriched in 15N (delta-15N = 1122). The magnetic fraction is very similar to the bulk sample in terms of both nitrogen release pattern and isotopic profile; the non-magnetic fraction contains significantly less heavy N. Carbon released at high temperatures shows a relatively heavy isotope signature. Similarly to CBb chondrites, ~20% of Fe,Ni-metal grains in Isheyevo are chemically zoned. Similarly to CH chondrites, some metal grains are Ni-rich (>20 wt% Ni). In contrast to CBb and CH chondrites, most metal grains are thermally decomposed into Ni-rich and Ni-poor phases. Similar to CH chondrites, chondrules have porphyritic and non-porphyritic textures and ferromagnesian (type I and II), silica-rich, and aluminum-rich bulk compositions. Some of the layered ferromagnesian chondrules are surrounded by ferrous olivine or phyllosilicate rims. Phyllosilicates in chondrule rims are compositionally distinct from those in the hydrated lithic clasts. Similarly to CH chondrites, CAIs are dominated by the hibonite-, grossite-, and melilite-rich types; AOAs are very rare. We infer that Isheyevo is a complex mixture of materials formed by different processes and under different physico-chemical conditions. Chondrules and refractory inclusions of two populations, metal grains, and heavily hydrated clasts accreted together into the Isheyevo parent asteroid in a region of the protoplanetary disk depleted in fine-grained dust. Such a scenario is consistent with the presence of solar windimplanted noble gases in Isheyevo and with its comparatively old K-Ar age. We cannot exclude that the K-Ar system was affected by a later collisional event. The cosmic-ray exposure (CRE) age of Isheyevo determined by cosmogenic 38Ar is ~34 Ma, similar to that of the Bencubbin (CBa) meteorite.
2008-01-01T00:00:00Z