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Origin of opaque assemblages in C3V meteorites: Implications for nebular and planetary processes

Blum, Joel D. and Wasserburg, G. J. and Hutcheon, I. D. and Beckett, J. R. and Stolper, E. M. (1989) Origin of opaque assemblages in C3V meteorites: Implications for nebular and planetary processes. Geochimica et Cosmochimica Acta, 53 (2). pp. 543-556. ISSN 0016-7037. http://resolver.caltech.edu/CaltechAUTHORS:20120821-154919308

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Abstract

Mineral phases from opaque assemblages (OAs) in Ca, Al-rich refractory inclusions (CAIs), chondrules and matrix in C3V meteoites were chemically analyzed and compared with experimentally determined phase equilibria and partitioning data in the Ni-Fe-S, Ni-Fe-S and Ni-Fe-O systems to estimate the temperature, sulfur fugacity (f_(S2)) and oxygen (f_(O2)) of OA formation. The kinetics of dissolution and exsolution of metallic phases in the Ni-Fe-Ru system were used to constrain the thermal history of OAss that occur in CAIs. Based on this work, we suggest that OAs formed after the crystallization of host CAIs by exsolution, sulfidation and oxidation of precursor alloys at low temperatures (~ 770 K) and higher than solar gas f_(S2) and f_(S2). Our model contrasts with previous models that call upon the formation of CAI OAs by aggregation of previously formed phases in the solar nebula prior to the crystallization of CAIs. Opaque assemblages in CAIs and chondrules probably originated as homogeneous alloys during melting of the silicate protions of CAIs and chondrules. The compositions of these precursor alloys reflect high-temperature and low-f_(O2) conditions in the early solar nebula. The similarities in the temperature, f_(S2) and f_(O2) of equilibrium for OAs that occur in CAIs, chondrules and matrix suggest that these three components of C3V meteorites share a common, late low-temperature history. The mineral phases in OAs do not preserve an independent history prior to CAI and chondrule melting and crystallization, but instead provide important information on the post-accretionary history of C3V meteorites and allow us to quantify the temperature, f_(S2) and f_(O2) of cooling planetary environments.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1016/0016-7037(89)90404-3DOIUNSPECIFIED
http://www.sciencedirect.com/science/article/pii/0016703789904043PublisherUNSPECIFIED
Additional Information:© 1989 Pergamon Press. Received 27 July 1988. Accepted 18 November 1988. Available online 27 March 2003. We thank H. Palme and J. T. Armstrong for helpful discussions, S. E. Haggerty, K. C. Misra and an anonymous referee for reviews, and H. Palme, K. Keil and the U.S. Museum of Natural History for loaning us the meteorite specimens used in this study. Funding was provided by NASA Grants NAG 9-43 and NAG 9-105 and NSF Grant EAR 86-18526. Division Contribution No. 4664(631). Editorial handling: H. Y. McSween, Jr.
Funders:
Funding AgencyGrant Number
NASANAG 9-43
NASANAG 9-105
NSFEAR 86-18526
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Other Numbering System NameOther Numbering System ID
Caltech Division of Geological and Planetary Sciences4664
Lunatic Asylum Lab631
Record Number:CaltechAUTHORS:20120821-154919308
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20120821-154919308
Official Citation:Joel D. Blum, G.J. Wasserburg, I.D. Hutcheon, J.R. Beckett, E.M. Stolper, Origin of opaque assemblages in C3V meteorites: Implications for nebular and planetary processes, Geochimica et Cosmochimica Acta, Volume 53, Issue 2, February 1989, Pages 543-556, ISSN 0016-7037, 10.1016/0016-7037(89)90404-3. (http://www.sciencedirect.com/science/article/pii/0016703789904043)
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:33426
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:23 Aug 2012 16:49
Last Modified:29 Oct 2013 16:48

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