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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

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