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Oxygen Line Formation in 3D Hydrodynamical Model Atmospheres

Published online by Cambridge University Press:  30 March 2016

Martin Asplund
Martin Asplund*
Affiliation:
Astronomiska Observatoriet, Box 515, SE-751 20 Uppsala, Sweden

Abstract

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The formation of [Oɪ], Oɪ and OH lines in metal-poor stars has been studied by means of 3D hydrodynamical model atmospheres. For Oɪ detailed 3D non-LTE calculations have been performed. While the influence of 3D model atmospheres is minor for [Oɪ] and Oɪ lines, the very low temperatures encountered at low metallicities have a drastic impact on OH. As a result, the derived O abundances are found to be systematically overestimated in 1D analyses, casting doubts on the recent claims for a monotonic increase in [O/Fe] towards lower metallicities.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 12: Highlights of Astronomy. As presented at the XXIVth General Assembly of the IAU, 2000 , 2002 , pp. 432 - 434
Copyright
Copyright © Astronomical Society of Pacific 2002

References

Asplund, M., et al., 1999, A&A, 346, L17 Google Scholar
Asplund, M., et al., 2000a, A&A, 359, 729 Google Scholar
Asplund, M., et al., 2000b, A&A, 359, 743 Google Scholar
Asplund, M., García Pérez, A.E., 2000, submitted to A&A Google Scholar
Boesgaard, A.M., et al., 1999, AJ, 117, 492 Google Scholar
Botnen, A.V., 1997, Cand. Sci. thesis, University of Oslo Google Scholar
Israelian, G., et al., 1998, ApJ, 507, 805 Google Scholar
Stein, R.F., Nordlund, Å., 1998, ApJ, 499, 914 Google Scholar