Oxygen Abundances in Metal Poor Subgiant Stars from the O I Triplet

Details Oxygen Abundances in Metal Poor Subgiant Stars from the O I Triplet Oxygen Abundances in Metal Poor Subgiant Stars from the O I Triplet

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997pasp..109..226c&link_type=abstract

Publications of the Astronomical Society of the Pacific, v.109, p.226-235

Astronomy and Astrophysics

Astronomy

57

Stars: Abundances, Galaxy: Halo

Scientific paper

This paper examines the oxygen abundance of 24 main-sequence turn-off and subgiant stars through the permitted O I triplet near $\lambda$7774 {\AA}. In agreement with prior investigators, we find that the O abundance from the triplet is about 0.53 dex higher than is typically found from other means such as the [O I] $\lambda$6300 {\AA} line or the UV and IR bands from OH. Our average [O/Fe] is +0.79 $\pm$ 0.29 (1 $\sigma$), with the uncertainties in the individual methods being dominated by systematic errors in our incomplete understanding of the formation of these high excitation lines under non-LTE conditions. Several methods of resolving the on-going discrepancy are discussed in detail. We find that the problem is not fixed by simply changing the model atmosphere parameters, and that the best methods seem to require a detailed non-LTE analysis based on both the structure of the oxygen atom and the source function within and above the photosphere. The trend of increasing O with decreasing Fe is briefly explored and is found to be qualitatively consistent with other works. (SECTION: Stars)

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