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  • 1
    Publication Date: 2000-05-08
    Description: Chemical zoning patterns in some iron, nickel metal grains from CH carbonaceous chondrites imply formation at temperatures from 1370 to 1270 kelvin by condensation from a solar nebular gas cooling at a rate of approximately 0.2 kelvin per hour. This cooling rate requires a large-scale thermal event in the nebula, in contrast to the localized, transient heating events inferred for chondrule formation. In our model, mass accretion through the protoplanetary disk caused large-scale evaporation of precursor dust near its midplane inside of a few astronomical units. Gas convectively moved from the midplane to cooler regions above it, and the metal grains condensed in these parcels of rising gas.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Meibom -- Desch -- Krot -- Cuzzi -- Petaev -- Wilson -- Keil -- New York, N.Y. -- Science. 2000 May 5;288(5467):839-41.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Hawai'i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawai'i at Manoa, Honolulu, HI 96822, USA. NASA Ames Research Center, Mail Stop 245-3, Moffett Field, CA 94035, USA. Harvard-Smithson.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/10797001" target="_blank"〉PubMed〈/a〉
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  • 2
    Publication Date: 2001-03-07
    Description: Chondrules in the metal-rich meteorites Hammadah al Hamra 237 and QUE 94411 have recorded highly energetic thermal events that resulted in complete vaporization of a dusty region of the solar nebula (dust/gas ratio of about 10 to 50 times solar). These chondrules formed under oxidizing conditions before condensation of iron-nickel metal, at temperatures greater than or equal to 1500 K, and were isolated from the cooling gas before condensation of moderately volatile elements such as manganese, sodium, potassium, and sulfur. This astrophysical environment is fundamentally different from conventional models for chondrule formation by localized, brief, repetitive heating events that resulted in incomplete melting of solid precursors initially residing at ambient temperatures below approximately 650 K.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Krot, A N -- Meibom, A -- Russell, S S -- Alexander, C M -- Jeffries, T E -- Keil, K -- New York, N.Y. -- Science. 2001 Mar 2;291(5509):1776-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Hawai'i Institute of Geophysics and Planetology (HIGP), School of Ocean and Earth Science and Technology (SOEST), University of Hawai'i at Manoa, Honolulu, HI 96822, USA. sasha@pgd.hawaii.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11230691" target="_blank"〉PubMed〈/a〉
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  • 3
    Publication Date: 2002-09-07
    Description: The lead-lead isochron age of chondrules in the CR chondrite Acfer 059 is 4564.7 +/- 0.6 million years ago (Ma), whereas the lead isotopic age of calcium-aluminum-rich inclusions (CAIs) in the CV chondrite Efremovka is 4567.2 +/- 0.6 Ma. This gives an interval of 2.5 +/- 1.2 million years (My) between formation of the CV CAIs and the CR chondrules and indicates that CAI- and chondrule-forming events lasted for at least 1.3 My. This time interval is consistent with a 2- to 3-My age difference between CR CAIs and chondrules inferred from the differences in their initial 26Al/27Al ratios and supports the chronological significance of the 26Al-26Mg systematics.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Amelin, Yuri -- Krot, Alexander N -- Hutcheon, Ian D -- Ulyanov, Alexander A -- New York, N.Y. -- Science. 2002 Sep 6;297(5587):1678-83.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Earth Sciences, Royal Ontario Museum, Toronto, ON M5S 2C6, Canada. yamelin@NRCan.gc.ca〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/12215641" target="_blank"〉PubMed〈/a〉
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  • 4
    Publication Date: 2006-12-16
    Description: The bulk of the comet 81P/Wild 2 (hereafter Wild 2) samples returned to Earth by the Stardust spacecraft appear to be weakly constructed mixtures of nanometer-scale grains, with occasional much larger (over 1 micrometer) ferromagnesian silicates, Fe-Ni sulfides, Fe-Ni metal, and accessory phases. The very wide range of olivine and low-Ca pyroxene compositions in comet Wild 2 requires a wide range of formation conditions, probably reflecting very different formation locations in the protoplanetary disk. The restricted compositional ranges of Fe-Ni sulfides, the wide range for silicates, and the absence of hydrous phases indicate that comet Wild 2 experienced little or no aqueous alteration. Less abundant Wild 2 materials include a refractory particle, whose presence appears to require radial transport in the early protoplanetary disk.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Zolensky, Michael E -- Zega, Thomas J -- Yano, Hajime -- Wirick, Sue -- Westphal, Andrew J -- Weisberg, Mike K -- Weber, Iris -- Warren, Jack L -- Velbel, Michael A -- Tsuchiyama, Akira -- Tsou, Peter -- Toppani, Alice -- Tomioka, Naotaka -- Tomeoka, Kazushige -- Teslich, Nick -- Taheri, Mitra -- Susini, Jean -- Stroud, Rhonda -- Stephan, Thomas -- Stadermann, Frank J -- Snead, Christopher J -- Simon, Steven B -- Simionovici, Alexandre -- See, Thomas H -- Robert, Francois -- Rietmeijer, Frans J M -- Rao, William -- Perronnet, Murielle C -- Papanastassiou, Dimitri A -- Okudaira, Kyoko -- Ohsumi, Kazumasa -- Ohnishi, Ichiro -- Nakamura-Messenger, Keiko -- Nakamura, Tomoki -- Mostefaoui, Smail -- Mikouchi, Takashi -- Meibom, Anders -- Matrajt, Graciela -- Marcus, Matthew A -- Leroux, Hugues -- Lemelle, Laurence -- Le, Loan -- Lanzirotti, Antonio -- Langenhorst, Falko -- Krot, Alexander N -- Keller, Lindsay P -- Kearsley, Anton T -- Joswiak, David -- Jacob, Damien -- Ishii, Hope -- Harvey, Ralph -- Hagiya, Kenji -- Grossman, Lawrence -- Grossman, Jeffrey N -- Graham, Giles A -- Gounelle, Matthieu -- Gillet, Philippe -- Genge, Matthew J -- Flynn, George -- Ferroir, Tristan -- Fallon, Stewart -- Fakra, Sirine -- Ebel, Denton S -- Dai, Zu Rong -- Cordier, Patrick -- Clark, Benton -- Chi, Miaofang -- Butterworth, Anna L -- Brownlee, Donald E -- Bridges, John C -- Brennan, Sean -- Brearley, Adrian -- Bradley, John P -- Bleuet, Pierre -- Bland, Phil A -- Bastien, Ron -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1735-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA. michael.e.zolensky@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170295" target="_blank"〉PubMed〈/a〉
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  • 5
    Publication Date: 2007-06-16
    Description: Oxygen isotopic composition of our solar system is believed to have resulted from mixing of two isotopically distinct nebular reservoirs, 16O-rich and (17,18)O-rich relative to Earth. The nature and composition of the (17,18)O-rich reservoir are poorly constrained. We report an in situ discovery of a chemically and isotopically unique material distributed ubiquitously in fine-grained matrix of a primitive carbonaceous chondrite Acfer 094. This material formed by oxidation of Fe,Ni-metal and sulfides by water either in the solar nebula or on a planetesimal. Oxygen isotopic composition of this material indicates that the water was highly enriched in 17O and 18O (delta(17,18)O(SMOW) = +180 per thousand per mil), providing the first evidence for an extremely (17,18)O-rich reservoir in the early solar system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sakamoto, Naoya -- Seto, Yusuke -- Itoh, Shoichi -- Kuramoto, Kiyoshi -- Fujino, Kiyoshi -- Nagashima, Kazuhide -- Krot, Alexander N -- Yurimoto, Hisayoshi -- New York, N.Y. -- Science. 2007 Jul 13;317(5835):231-3. Epub 2007 Jun 14.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Natural History Sciences, Hokkaido University, Sapporo 060-0810, Japan.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17569827" target="_blank"〉PubMed〈/a〉
    Keywords: *Meteoroids ; Oxidation-Reduction ; Oxygen/*analysis ; Oxygen Isotopes/*analysis ; *Solar System ; Water/*chemistry
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  • 6
    Publication Date: 2012-11-03
    Description: Transient heating events that formed calcium-aluminum-rich inclusions (CAIs) and chondrules are fundamental processes in the evolution of the solar protoplanetary disk, but their chronology is not understood. Using U-corrected Pb-Pb dating, we determined absolute ages of individual CAIs and chondrules from primitive meteorites. CAIs define a brief formation interval corresponding to an age of 4567.30 +/- 0.16 million years (My), whereas chondrule ages range from 4567.32 +/- 0.42 to 4564.71 +/- 0.30 My. These data refute the long-held view of an age gap between CAIs and chondrules and, instead, indicate that chondrule formation started contemporaneously with CAIs and lasted ~3 My. This time scale is similar to disk lifetimes inferred from astronomical observations, suggesting that the formation of CAIs and chondrules reflects a process intrinsically linked to the secular evolution of accretionary disks.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Connelly, James N -- Bizzarro, Martin -- Krot, Alexander N -- Nordlund, Ake -- Wielandt, Daniel -- Ivanova, Marina A -- New York, N.Y. -- Science. 2012 Nov 2;338(6107):651-5. doi: 10.1126/science.1226919.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Centre for Star and Planet Formation and Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark. connelly@snm.ku.dk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23118187" target="_blank"〉PubMed〈/a〉
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  • 7
    Publication Date: 1998-12-04
    Description: Fayalite grains in chondrules in the oxidized, aqueously altered CV3 chondrite Mokoia have large excesses of radiogenic chromium-53. These excesses indicate the in situ decay of short-lived manganese-53 (half-life = 3.7 million years) and define an initial 53Mn/55Mn ratio of 2.32 (+/-0.18) x 10(-6). This ratio is comparable to values for carbonates in CI and CM chondrites and for several classes of differentiated meteorites. Mokoia fayalites formed 7 to 16 million years after Allende calcium-aluminum-rich inclusions, during hydrothermal activity on a geologically active asteroid after chondritic components had ceased forming in the solar nebula.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hutcheon, I D -- Krot, A N -- Keil, K -- Phinney, D L -- Scott, E R -- New York, N.Y. -- Science. 1998 Dec 4;282(5395):1865-7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lawrence Livermore National Laboratory (LLNL), Livermore, CA 94551, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9836631" target="_blank"〉PubMed〈/a〉
    Keywords: Chromium Isotopes/analysis ; Manganese/analysis ; *Meteoroids ; *Minor Planets ; Oxides/analysis ; Radioisotopes
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  • 8
    Publication Date: 2002-02-09
    Description: Carbonaceous chondrite condensate olivine grains from two distinct petrographic settings, calcium-aluminum-rich inclusion (CAI) accretionary rims and amoeboid olivine aggregates (AOAs), are oxygen-16 (16O) enriched at the level previously observed inside CAIs. This requires that the gas in the nebular region where these grains condensed was 16O-rich. This contrasts with an 16O-poor gas present during the formation of chondrules, suggesting that CAIs and AOAs formed in a spatially restricted region of the solar nebula containing 16O-rich gas. The 16O-rich gas composition may have resulted either from mass-independent isotopic chemistry or from evaporation of regions with enhanced dust/gas ratios, possibly in an X-wind environment near the young Sun.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Krot, Alexander N -- McKeegan, Kevin D -- Leshin, Laurie A -- MacPherson, Glenn J -- Scott, Edward R D -- New York, N.Y. -- Science. 2002 Feb 8;295(5557):1051-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Hawaii Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawaii, Honolulu, HI 96822, USA. sasha@higp.hawaii.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11834830" target="_blank"〉PubMed〈/a〉
    Keywords: Aluminum/analysis ; Calcium/analysis ; Cosmic Dust ; Evolution, Chemical ; Gases ; Iron Compounds ; Magnesium Compounds ; *Meteoroids ; Minerals/analysis ; Oxygen/*analysis ; Oxygen Isotopes/analysis ; Silicates ; *Solar System
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  • 9
    Publication Date: 2009-04-18
    Description: Stable-isotope variations exist among inner solar system solids, planets, and asteroids, but their importance is not understood. We report correlated, mass-independent variations of titanium-46 and titanium-50 in bulk analyses of these materials. Because titanium-46 and titanium-50 have different nucleosynthetic origins, this correlation suggests that the presolar dust inherited from the protosolar molecular cloud was well mixed when the oldest solar system solids formed, but requires a subsequent process imparting isotopic variability at the planetary scale. We infer that thermal processing of molecular cloud material, probably associated with volatile-element depletions in the inner solar system, resulted in selective destruction of thermally unstable, isotopically anomalous presolar components, producing residual isotopic heterogeneity. This implies that terrestrial planets accreted from thermally processed solids with nonsolar isotopic compositions.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Trinquier, Anne -- Elliott, Tim -- Ulfbeck, David -- Coath, Christopher -- Krot, Alexander N -- Bizzarro, Martin -- New York, N.Y. -- Science. 2009 Apr 17;324(5925):374-6. doi: 10.1126/science.1168221.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Center for Stars and Planets, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19372428" target="_blank"〉PubMed〈/a〉
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  • 10
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    American Association for the Advancement of Science (AAAS)
    Publication Date: 2011-08-27
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Krot, Alexander N -- New York, N.Y. -- Science. 2011 Aug 26;333(6046):1098-9. doi: 10.1126/science.1212145.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Manoa, Honolulu, HI 96822, USA. sasha@higp.hawaii.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21868659" target="_blank"〉PubMed〈/a〉
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