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Accretion and Preservation of D-rich Organic Particles in Carbonaceous Chondrites: Evidence for Important Transport in the Early Solar System Nebula

Remusat, L. and Guan, Y. and Wang, Y. and Eiler, J. M. (2010) Accretion and Preservation of D-rich Organic Particles in Carbonaceous Chondrites: Evidence for Important Transport in the Early Solar System Nebula. Astrophysical Journal, 713 (2). pp. 1048-1058. ISSN 0004-637X.

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We have acquired NanoSIMS images of the matrices of CI, CM, and CR carbonaceous chondrites to study, in situ, the organic matter trapped during the formation of their parent bodies. D/H ratio images reveal the occurrence of D-rich hot spots, constituting isolated organic particles. Not all the organic particles are D-rich hot spots, indicating that at least two kinds of organic particles have been accreted in the parent bodies. Ratio profiles through D-rich hot spots indicate that no significant self-diffusion of deuterium occurs between the D-rich organic matter and the depleted hydrous minerals that are surrounding them. This is not the result of a physical shielding by any constituent of the chondrites. Ab initio calculations indicate that it cannot be explained by isotopic equilibrium. Then it appears that the organic matter that is extremely enriched in D does not exchange with the hydrous minerals, or this exchange is so slow that it is not significant over the 4.5 billion year history on the parent body. If we consider that the D-rich hot spots are the result of an exposure to intense irradiation, then it appears that carbonaceous chondrites accreted organic particles that have been brought to different regions of the solar nebula. This is likely the result of important radial and vertical transport in the early solar system.

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Guan, Y.0000-0002-7636-3735
Additional Information:© 2010 American Astronomical Society. Received 2009 November 11; accepted 2010 March 2; published 2010 March 30. Fran¸cois Robert and Weifu Guo are thanked for providing samples. We also thank Alex Session for helpful discussions. L.R. is grateful to Nivedita Thiagarajan for her useful comments on the manuscript and illustrations. This paper was improved thanks to comments from an anonymous referee.
Subject Keywords:astrochemistry; meteorites, meteors, meteoroids; protoplanetary disks
Issue or Number:2
Classification Code:PACS: 96.55.+z; 96.30.Za; 96.10.+i
Record Number:CaltechAUTHORS:20100607-120524366
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Official Citation:L. Remusat et al 2010 ApJ 713 1048 doi: 10.1088/0004-637X/713/2/1048
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:18579
Deposited By: Jason Perez
Deposited On:09 Jun 2010 20:18
Last Modified:26 Nov 2019 23:44

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