Other
Scientific paper
Jan 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999m%26ps...34...99w&link_type=abstract
Meteoritics & Planetary Science, vol. 34, no. 1, pp. 99-107 (1999).
Other
28
Scientific paper
The outer layers of the Sun are thought to preserve the average isotopic and chemical composition of the solar system. The solar oxygen 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 CAI 16O line between ((18O, (17O) = (16.4, 11.4)=89 and (12.3, 7.5)=89. Consideration of data from ordinary chondrites suggests that the range of predicted solar composition should extend to slightly lower (18O 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 ((18O, (17O) values along an extension of the CAI 16O line to (33, 28)=89. The model is also sensitive to the nebular oxygen gas phase. If conversion of most of the gaseous oxygen from CO to H2O 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 oxygen component is discussed. A distribution of initial solid compositions along the CAI 16O 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. A measurement of the solar oxygen composition to a precision of several permil would thus clearly distinguish between these theories, and should clarify a number of other important issues regarding solar system formation.
Burnett Don S.
Huss Gary R.
Wiens Roger C.
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