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  • 1
    Publication Date: 1992-12-04
    Description: One hypothesis for the origin of the nanometer-size diamonds found at the Cretaceous-Tertiary (K-T) boundary is that they are relict interstellar diamond grains carried by a postulated asteroid. The (13)C/(12)C and (15)N/(14)N ratios of the diamonds from two sites in North America, however, show that the diamonds are two component mixtures differing in carbon and nitrogen isotopic composition and nitrogen abundance. Samples from a site from Italy show no evidence for either diamond component. All the isotopic signatures obtained from the K-T boundary are material well distinguished from known meteoritic diamonds, particularly the fine-grain interstellar diamonds that are abundant in primitive chondrites. The K-T diamonds were most likely produced during the impact of the asteroid with Earth or in a plasma resulting from the associated fireball.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gilmour, I -- Russell, S S -- Arden, J W -- Lee, M R -- Franchi, I A -- Pillinger, C T -- New York, N.Y. -- Science. 1992 Dec 4;258(5088):1624-6.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17742530" target="_blank"〉PubMed〈/a〉
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  • 2
    Publication Date: 2006-08-26
    Description: Asteroidal material, delivered to Earth as meteorites, preserves a record of the earliest stages of planetary formation. High-precision oxygen isotope analyses for the two major groups of stony-iron meteorites (main-group pallasites and mesosiderites) demonstrate that each group is from a distinct asteroidal source. Mesosiderites are isotopically identical to the howardite-eucrite-diogenite clan and, like them, are probably derived from the asteroid 4 Vesta. Main-group pallasites represent intermixed core-mantle material from a single disrupted asteroid and have no known equivalents among the basaltic meteorites. The stony-iron meteorites demonstrate that intense asteroidal deformation accompanied planetary accretion in the early Solar System.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Greenwood, R C -- Franchi, I A -- Jambon, A -- Barrat, J A -- Burbine, T H -- New York, N.Y. -- Science. 2006 Sep 22;313(5794):1763-5. Epub 2006 Aug 24.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Planetary and Space Sciences Research Institute, Open University, Walton Hall, Milton Keynes, MK7 6AA UK. r.c.greenwood@open.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16931721" target="_blank"〉PubMed〈/a〉
    Keywords: *Evolution, Planetary ; *Meteoroids ; *Minor Planets ; *Oxygen Isotopes
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  • 3
    Publication Date: 2006-12-16
    Description: The Stardust spacecraft collected thousands of particles from comet 81P/Wild 2 and returned them to Earth for laboratory study. The preliminary examination of these samples shows that the nonvolatile portion of the comet is an unequilibrated assortment of materials that have both presolar and solar system origin. The comet contains an abundance of silicate grains that are much larger than predictions of interstellar grain models, and many of these are high-temperature minerals that appear to have formed in the inner regions of the solar nebula. Their presence in a comet proves that the formation of the solar system included mixing on the grandest scales.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Brownlee, Don -- Tsou, Peter -- Aleon, Jerome -- Alexander, Conel M O'd -- Araki, Tohru -- Bajt, Sasa -- Baratta, Giuseppe A -- Bastien, Ron -- Bland, Phil -- Bleuet, Pierre -- Borg, Janet -- Bradley, John P -- Brearley, Adrian -- Brenker, F -- Brennan, Sean -- Bridges, John C -- Browning, Nigel D -- Brucato, John R -- Bullock, E -- Burchell, Mark J -- Busemann, Henner -- Butterworth, Anna -- Chaussidon, Marc -- Cheuvront, Allan -- Chi, Miaofang -- Cintala, Mark J -- Clark, B C -- Clemett, Simon J -- Cody, George -- Colangeli, Luigi -- Cooper, George -- Cordier, Patrick -- Daghlian, C -- Dai, Zurong -- D'Hendecourt, Louis -- Djouadi, Zahia -- Dominguez, Gerardo -- Duxbury, Tom -- Dworkin, Jason P -- Ebel, Denton S -- Economou, Thanasis E -- Fakra, Sirine -- Fairey, Sam A J -- Fallon, Stewart -- Ferrini, Gianluca -- Ferroir, T -- Fleckenstein, Holger -- Floss, Christine -- Flynn, George -- Franchi, Ian A -- Fries, Marc -- Gainsforth, Z -- Gallien, J-P -- Genge, Matt -- Gilles, Mary K -- Gillet, Philipe -- Gilmour, Jamie -- Glavin, Daniel P -- Gounelle, Matthieu -- Grady, Monica M -- Graham, Giles A -- Grant, P G -- Green, Simon F -- Grossemy, Faustine -- Grossman, Lawrence -- Grossman, Jeffrey N -- Guan, Yunbin -- Hagiya, Kenji -- Harvey, Ralph -- Heck, Philipp -- Herzog, Gregory F -- Hoppe, Peter -- Horz, Friedrich -- Huth, Joachim -- Hutcheon, Ian D -- Ignatyev, Konstantin -- Ishii, Hope -- Ito, Motoo -- Jacob, Damien -- Jacobsen, Chris -- Jacobsen, Stein -- Jones, Steven -- Joswiak, David -- Jurewicz, Amy -- Kearsley, Anton T -- Keller, Lindsay P -- Khodja, H -- Kilcoyne, A L David -- Kissel, Jochen -- Krot, Alexander -- Langenhorst, Falko -- Lanzirotti, Antonio -- Le, Loan -- Leshin, Laurie A -- Leitner, J -- Lemelle, L -- Leroux, Hugues -- Liu, Ming-Chang -- Luening, K -- Lyon, Ian -- Macpherson, Glen -- Marcus, Matthew A -- Marhas, Kuljeet -- Marty, Bernard -- Matrajt, Graciela -- McKeegan, Kevin -- Meibom, Anders -- Mennella, Vito -- Messenger, Keiko -- Messenger, Scott -- Mikouchi, Takashi -- Mostefaoui, Smail -- Nakamura, Tomoki -- Nakano, T -- Newville, M -- Nittler, Larry R -- Ohnishi, Ichiro -- Ohsumi, Kazumasa -- Okudaira, Kyoko -- Papanastassiou, Dimitri A -- Palma, Russ -- Palumbo, Maria E -- Pepin, Robert O -- Perkins, David -- Perronnet, Murielle -- Pianetta, P -- Rao, William -- Rietmeijer, Frans J M -- Robert, Francois -- Rost, D -- Rotundi, Alessandra -- Ryan, Robert -- Sandford, Scott A -- Schwandt, Craig S -- See, Thomas H -- Schlutter, Dennis -- Sheffield-Parker, J -- Simionovici, Alexandre -- Simon, Steven -- Sitnitsky, I -- Snead, Christopher J -- Spencer, Maegan K -- Stadermann, Frank J -- Steele, Andrew -- Stephan, Thomas -- Stroud, Rhonda -- Susini, Jean -- Sutton, S R -- Suzuki, Y -- Taheri, Mitra -- Taylor, Susan -- Teslich, Nick -- Tomeoka, Kazu -- Tomioka, Naotaka -- Toppani, Alice -- Trigo-Rodriguez, Josep M -- Troadec, David -- Tsuchiyama, Akira -- Tuzzolino, Anthony J -- Tyliszczak, Tolek -- Uesugi, K -- Velbel, Michael -- Vellenga, Joe -- Vicenzi, E -- Vincze, L -- Warren, Jack -- Weber, Iris -- Weisberg, Mike -- Westphal, Andrew J -- Wirick, Sue -- Wooden, Diane -- Wopenka, Brigitte -- Wozniakiewicz, Penelope -- Wright, Ian -- Yabuta, Hikaru -- Yano, Hajime -- Young, Edward D -- Zare, Richard N -- Zega, Thomas -- Ziegler, Karen -- Zimmerman, Laurent -- Zinner, Ernst -- Zolensky, Michael -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1711-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of Washington, Seattle, WA 98195, USA. brownlee@astro.washington.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170289" target="_blank"〉PubMed〈/a〉
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  • 4
    Publication Date: 2006-12-16
    Description: Organics found in comet 81P/Wild 2 samples show a heterogeneous and unequilibrated distribution in abundance and composition. Some organics are similar, but not identical, to those in interplanetary dust particles and carbonaceous meteorites. A class of aromatic-poor organic material is also present. The organics are rich in oxygen and nitrogen compared with meteoritic organics. Aromatic compounds are present, but the samples tend to be relatively poorer in aromatics than are meteorites and interplanetary dust particles. The presence of deuterium and nitrogen-15 excesses suggest that some organics have an interstellar/protostellar heritage. Although the variable extent of modification of these materials by impact capture is not yet fully constrained, a diverse suite of organic compounds is present and identifiable within the returned samples.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sandford, Scott A -- Aleon, Jerome -- Alexander, Conel M O'd -- Araki, Tohru -- Bajt, Sasa -- Baratta, Giuseppe A -- Borg, Janet -- Bradley, John P -- Brownlee, Donald E -- Brucato, John R -- Burchell, Mark J -- Busemann, Henner -- Butterworth, Anna -- Clemett, Simon J -- Cody, George -- Colangeli, Luigi -- Cooper, George -- D'Hendecourt, Louis -- Djouadi, Zahia -- Dworkin, Jason P -- Ferrini, Gianluca -- Fleckenstein, Holger -- Flynn, George J -- Franchi, Ian A -- Fries, Marc -- Gilles, Mary K -- Glavin, Daniel P -- Gounelle, Matthieu -- Grossemy, Faustine -- Jacobsen, Chris -- Keller, Lindsay P -- Kilcoyne, A L David -- Leitner, Jan -- Matrajt, Graciela -- Meibom, Anders -- Mennella, Vito -- Mostefaoui, Smail -- Nittler, Larry R -- Palumbo, Maria E -- Papanastassiou, Dimitri A -- Robert, Francois -- Rotundi, Alessandra -- Snead, Christopher J -- Spencer, Maegan K -- Stadermann, Frank J -- Steele, Andrew -- Stephan, Thomas -- Tsou, Peter -- Tyliszczak, Tolek -- Westphal, Andrew J -- Wirick, Sue -- Wopenka, Brigitte -- Yabuta, Hikaru -- Zare, Richard N -- Zolensky, Michael E -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1720-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astrophysics Branch, NASA-Ames Research Center, Moffett Field, CA 94035, USA. ssandford@mail.arc.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170291" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon/analysis ; Cosmic Dust/analysis ; Deuterium/analysis ; *Meteoroids ; Nitrogen/analysis ; Nitrogen Isotopes/analysis ; Organic Chemicals/*analysis ; Oxygen/analysis ; Polycyclic Hydrocarbons, Aromatic/analysis ; Spacecraft
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  • 5
    Publication Date: 2006-12-16
    Description: We measured the elemental compositions of material from 23 particles in aerogel and from residue in seven craters in aluminum foil that was collected during passage of the Stardust spacecraft through the coma of comet 81P/Wild 2. These particles are chemically heterogeneous at the largest size scale analyzed ( approximately 180 ng). The mean elemental composition of this Wild 2 material is consistent with the CI meteorite composition, which is thought to represent the bulk composition of the solar system, for the elements Mg, Si, Mn, Fe, and Ni to 35%, and for Ca and Ti to 60%. The elements Cu, Zn, and Ga appear enriched in this Wild 2 material, which suggests that the CI meteorites may not represent the solar system composition for these moderately volatile minor elements.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Flynn, George J -- Bleuet, Pierre -- Borg, Janet -- Bradley, John P -- Brenker, Frank E -- Brennan, Sean -- Bridges, John -- Brownlee, Don E -- Bullock, Emma S -- Burghammer, Manfred -- Clark, Benton C -- Dai, Zu Rong -- Daghlian, Charles P -- Djouadi, Zahia -- Fakra, Sirine -- Ferroir, Tristan -- Floss, Christine -- Franchi, Ian A -- Gainsforth, Zack -- Gallien, Jean-Paul -- Gillet, Philippe -- Grant, Patrick G -- Graham, Giles A -- Green, Simon F -- Grossemy, Faustine -- Heck, Philipp R -- Herzog, Gregory F -- Hoppe, Peter -- Horz, Friedrich -- Huth, Joachim -- Ignatyev, Konstantin -- Ishii, Hope A -- Janssens, Koen -- Joswiak, David -- Kearsley, Anton T -- Khodja, Hicham -- Lanzirotti, Antonio -- Leitner, Jan -- Lemelle, Laurence -- Leroux, Hugues -- Luening, Katharina -- Macpherson, Glenn J -- Marhas, Kuljeet K -- Marcus, Matthew A -- Matrajt, Graciela -- Nakamura, Tomoki -- Nakamura-Messenger, Keiko -- Nakano, Tsukasa -- Newville, Matthew -- Papanastassiou, Dimitri A -- Pianetta, Piero -- Rao, William -- Riekel, Christian -- Rietmeijer, Frans J M -- Rost, Detlef -- Schwandt, Craig S -- See, Thomas H -- Sheffield-Parker, Julie -- Simionovici, Alexandre -- Sitnitsky, Ilona -- Snead, Christopher J -- Stadermann, Frank J -- Stephan, Thomas -- Stroud, Rhonda M -- Susini, Jean -- Suzuki, Yoshio -- Sutton, Stephen R -- Taylor, Susan -- Teslich, Nick -- Troadec, D -- Tsou, Peter -- Tsuchiyama, Akira -- Uesugi, Kentaro -- Vekemans, Bart -- Vicenzi, Edward P -- Vincze, Laszlo -- Westphal, Andrew J -- Wozniakiewicz, Penelope -- Zinner, Ernst -- Zolensky, Michael E -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1731-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, State University of New York at Plattsburgh, 101 Broad Street, Plattsburgh, NY 12901, USA. george.flynn@plattsburgh.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170294" target="_blank"〉PubMed〈/a〉
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  • 6
    Publication Date: 2012-10-16
    Description: Tissint (Morocco) is the fifth martian meteorite collected after it was witnessed falling to Earth. Our integrated mineralogical, petrological, and geochemical study shows that it is a depleted picritic shergottite similar to EETA79001A. Highly magnesian olivine and abundant glass containing martian atmosphere are present in Tissint. Refractory trace element, sulfur, and fluorine data for the matrix and glass veins in the meteorite indicate the presence of a martian surface component. Thus, the influence of in situ martian weathering can be unambiguously distinguished from terrestrial contamination in this meteorite. Martian weathering features in Tissint are compatible with the results of spacecraft observations of Mars. Tissint has a cosmic-ray exposure age of 0.7 +/- 0.3 million years, consistent with those of many other shergottites, notably EETA79001, suggesting that they were ejected from Mars during the same event.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Aoudjehane, H Chennaoui -- Avice, G -- Barrat, J-A -- Boudouma, O -- Chen, G -- Duke, M J M -- Franchi, I A -- Gattacceca, J -- Grady, M M -- Greenwood, R C -- Herd, C D K -- Hewins, R -- Jambon, A -- Marty, B -- Rochette, P -- Smith, C L -- Sautter, V -- Verchovsky, A -- Weber, P -- Zanda, B -- New York, N.Y. -- Science. 2012 Nov 9;338(6108):785-8. doi: 10.1126/science.1224514. Epub 2012 Oct 11.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Hassan II University Casablanca, Faculty of Sciences, Geosciences Appliquees a l'Ingenierie et l'Amenagement (GAIA) Laboratory, BP 5366 Maarif, Casablanca, Morocco. chennaoui_h@yahoo.fr〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23065902" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon Isotopes/analysis ; Iron Compounds/analysis ; Magnesium Compounds/analysis ; *Mars ; *Meteoroids ; Nitrogen Isotopes/analysis ; Oxygen Isotopes/analysis ; Silicates/analysis
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  • 7
    Publication Date: 2004-08-03
    Description: The lunar meteorite Sayh al Uhaymir 169 consists of an impact melt breccia extremely enriched with potassium, rare earth elements, and phosphorus [thorium, 32.7 parts per million (ppm); uranium, 8.6 ppm; potassium oxide, 0.54 weight percent], and adherent regolith. The isotope systematics of the meteorite record four lunar impact events at 3909 +/- 13 million years ago (Ma), approximately 2800 Ma, approximately 200 Ma, and 〈0.34 Ma, and collision with Earth sometime after 9.7 +/- 1.3 thousand years ago. With these data, we can link the impact-melt breccia to Imbrium and pinpoint the source region of the meteorite to the Lalande impact crater.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gnos, Edwin -- Hofmann, Beda A -- Al-Kathiri, Ali -- Lorenzetti, Silvio -- Eugster, Otto -- Whitehouse, Martin J -- Villa, Igor M -- Jull, A J Timothy -- Eikenberg, Jost -- Spettel, Bernhard -- Krahenbuhl, Urs -- Franchi, Ian A -- Greenwood, Richard C -- New York, N.Y. -- Science. 2004 Jul 30;305(5684):657-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institut fur Geologie, Universitat Bern, Baltzerstrasse 1, CH-3012 Bern, Switzerland. gnos@geo.unibe.ch〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15286369" target="_blank"〉PubMed〈/a〉
    Keywords: Crystallization ; Elements ; *Evolution, Planetary ; Isotopes ; Lead ; Metals, Rare Earth/analysis ; *Meteoroids ; *Moon ; Phosphorus/analysis ; Potassium/analysis ; Thorium/analysis ; Uranium/analysis
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  • 8
    Publication Date: 2006-12-16
    Description: Infrared spectra of material captured from comet 81P/Wild 2 by the Stardust spacecraft reveal indigenous aliphatic hydrocarbons similar to those in interplanetary dust particles thought to be derived from comets, but with longer chain lengths than those observed in the diffuse interstellar medium. Similarly, the Stardust samples contain abundant amorphous silicates in addition to crystalline silicates such as olivine and pyroxene. The presence of crystalline silicates in Wild 2 is consistent with mixing of solar system and interstellar matter. No hydrous silicates or carbonate minerals were detected, which suggests a lack of aqueous processing of Wild 2 dust.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Keller, Lindsay P -- Bajt, Sasa -- Baratta, Giuseppe A -- Borg, Janet -- Bradley, John P -- Brownlee, Don E -- Busemann, Henner -- Brucato, John R -- Burchell, Mark -- Colangeli, Luigi -- d'Hendecourt, Louis -- Djouadi, Zahia -- Ferrini, Gianluca -- Flynn, George -- Franchi, Ian A -- Fries, Marc -- Grady, Monica M -- Graham, Giles A -- Grossemy, Faustine -- Kearsley, Anton -- Matrajt, Graciela -- Nakamura-Messenger, Keiko -- Mennella, Vito -- Nittler, Larry -- Palumbo, Maria E -- Stadermann, Frank J -- Tsou, Peter -- Rotundi, Alessandra -- Sandford, Scott A -- Snead, Christopher -- Steele, Andrew -- Wooden, Diane -- Zolensky, Mike -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1728-31.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astromaterials Research and Exploration Science Directorate, Mail Code KR, NASA-Johnson Space Center, Houston, TX 77058, USA. lindsay.p.keller@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170293" target="_blank"〉PubMed〈/a〉
    Keywords: Cosmic Dust/analysis ; Hydrocarbons/*analysis ; *Meteoroids ; Silicates/*analysis ; Spacecraft ; Spectroscopy, Fourier Transform Infrared
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  • 9
    Publication Date: 2006-12-16
    Description: Particles emanating from comet 81P/Wild 2 collided with the Stardust spacecraft at 6.1 kilometers per second, producing hypervelocity impact features on the collector surfaces that were returned to Earth. The morphologies of these surprisingly diverse features were created by particles varying from dense mineral grains to loosely bound, polymineralic aggregates ranging from tens of nanometers to hundreds of micrometers in size. The cumulative size distribution of Wild 2 dust is shallower than that of comet Halley, yet steeper than that of comet Grigg-Skjellerup.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Horz, Friedrich -- Bastien, Ron -- Borg, Janet -- Bradley, John P -- Bridges, John C -- Brownlee, Donald E -- Burchell, Mark J -- Chi, Miaofang -- Cintala, Mark J -- Dai, Zu Rong -- Djouadi, Zahia -- Dominguez, Gerardo -- Economou, Thanasis E -- Fairey, Sam A J -- Floss, Christine -- Franchi, Ian A -- Graham, Giles A -- Green, Simon F -- Heck, Philipp -- Hoppe, Peter -- Huth, Joachim -- Ishii, Hope -- Kearsley, Anton T -- Kissel, Jochen -- Leitner, Jan -- Leroux, Hugues -- Marhas, Kuljeet -- Messenger, Keiko -- Schwandt, Craig S -- See, Thomas H -- Snead, Christopher -- Stadermann, Frank J 1st -- Stephan, Thomas -- Stroud, Rhonda -- Teslich, Nick -- Trigo-Rodriguez, Josep M -- Tuzzolino, A J -- Troadec, David -- Tsou, Peter -- Warren, Jack -- Westphal, Andrew -- Wozniakiewicz, Penelope -- Wright, Ian -- Zinner, Ernst -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1716-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA. friedrich.p.horz@jsc.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170290" target="_blank"〉PubMed〈/a〉
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  • 10
    Publication Date: 2009-09-19
    Description: Triangulated observations of fireballs allow us to determine orbits and fall positions for meteorites. The great majority of basaltic meteorites are derived from the asteroid 4 Vesta. We report on a recent fall that has orbital properties and an oxygen isotope composition that suggest a distinct parent body. Although its orbit was almost entirely contained within Earth's orbit, modeling indicates that it originated from the innermost main belt. Because the meteorite parent body would likely be classified as a V-type asteroid, V-type precursors for basaltic meteorites unrelated to Vesta may reside in the inner main belt. This starting location is in agreement with predictions of a planetesimal evolution model that postulates the formation of differentiated asteroids in the terrestrial planet region, with surviving fragments concentrated in the innermost main belt.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Bland, Philip A -- Spurny, Pavel -- Towner, Martin C -- Bevan, Alex W R -- Singleton, Andrew T -- Bottke, William F Jr -- Greenwood, Richard C -- Chesley, Steven R -- Shrbeny, Lukas -- Borovicka, Jiri -- Ceplecha, Zdenek -- McClafferty, Terence P -- Vaughan, David -- Benedix, Gretchen K -- Deacon, Geoff -- Howard, Kieren T -- Franchi, Ian A -- Hough, Robert M -- New York, N.Y. -- Science. 2009 Sep 18;325(5947):1525-7. doi: 10.1126/science.1174787.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉IARC, Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK. p.a.bland@imperial.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19762639" target="_blank"〉PubMed〈/a〉
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