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The solar oxygen-isotopic composition: Predictions and implications for solar nebula processes

Wiens, R. C. and Huss, G. R. and Burnett, D. S. (1999) The solar oxygen-isotopic composition: Predictions and implications for solar nebula processes. Meteoritics and Planetary Science, 34 (1). pp. 99-107. ISSN 1086-9379. doi:10.1111/j.1945-5100.1999.tb01735.x.

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The outer layers of the Sun are thought to preserve the average isotopic and chemical composition of the solar system. The solar O-isotopic composition is essentially unmeasured, though models based on variations in meteoritic materials yield several predictions. These predictions are reviewed and possible variations on these predictions are explored. In particular, the two-component mixing model of Clayton and Mayeda (1984) (slightly revised here) predicts solar compositions to lie along an extension of the calcium-aluminum-rich inclusion (CAI) ^(16)O line between (δ^(18)O, δ^(17)O) = (16.4, 11.4)%0 and (12.3, 7.5)%0. Consideration of data from ordinary chondrites suggests that the range of predicted solar composition should extend to slightly lower δ^(18)O values. The predicted solar composition is critically sensitive to the solid/gas ratio in the meteorite-forming region, which is often considered to be significantly enriched over solar composition. A factor of two solid/gas enrichment raises the predicted solar (δ^(18)O, δ^(17)O) values along an extension of the CAI ^(16)O line to (33, 28)%0. The model is also sensitive to the nebular O gas phase. If conversion of most of the gaseous O from CO to H_2O occurred at relatively low temperatures and was incomplete at the time of CM aqueous alteration, the predicted nebular gas composition (and hence the solar composition) would be isotopically heavier along a slope 1/2 line. The likelihood of having a single solid nebular O component is discussed. A distribution of initial solid compositions along the CAI ^(16)O line (rather than simply as an end-member) would not significantly change the predictions above in at least one scenario. Even considering these variations within the mixing model, the predicted range of solar compositions is distinct from that expected if the meteoritic variations are due to non-mass-dependent fractionation. Thus, a measurement of the solar O composition to a precision of several permil would clearly distinguish between these theories and should clarify a number of other important issues regarding solar system formation.

Item Type:Article
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URLURL TypeDescription
Wiens, R. C.0000-0002-3409-7344
Huss, G. R.0000-0003-4281-7839
Burnett, D. S.0000-0001-9521-8675
Additional Information:© 1999 The Meteoritical Society. Received 1998 March 18; accepted in revised form 1998 November 5. This work was partially supported by NASA grant NAGW-4182 and the Genesis Discovery mission. Helpful discussions and informal and formal reviews by R. N. Clayton, K. Lodders, M. H. Thiemens, J. T. Wasson, B-G. Choi, K. D. McKeegan, P. Bochsler, and P. Cassen are greatly appreciated. We are also gratekl for editorial assistance by L. Schultz.
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Genesis Discovery MissionUNSPECIFIED
Issue or Number:1
Record Number:CaltechAUTHORS:20141203-141124907
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Official Citation:WIENS, R. C., HUSS, G. R. and BURNETT, D. S. (1999), The solar oxygen-isotopic composition: Predictions and implications for solar nebula processes. Meteoritics & Planetary Science, 34: 99–107. doi: 10.1111/j.1945-5100.1999.tb01735.x
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:52349
Deposited By: Tony Diaz
Deposited On:03 Dec 2014 22:17
Last Modified:10 Nov 2021 19:24

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