Oxygen Line Formation in 3D Hydrodynamical Model Atmospheres

M. Asplund
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引用次数: 1

Abstract

The formation of [O I], O I and OH lines in metal-poor stars has been studied by means of 3D hydrodynamical model atmospheres. For O I detailed 3D non-LTE calculations have been performed. While the influence of 3D model atmospheres is minor for [O I] and O I lines, the very low temperatures encountered at low metallicities have a drastic impact on the OH lines. 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.
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三维流体动力学模型大气中的氧线形成
利用三维流体动力学模型研究了贫金属恒星中[O I]、O I和OH谱线的形成。对于O I,已经执行了详细的3D非lte计算。虽然三维模型大气对[O I]和O I谱线的影响较小,但在低金属丰度下遇到的极低温度对OH谱线的影响很大。结果发现,在一维分析中,导出的O丰度被系统性地高估了,这对最近关于[O/Fe]向低金属丰度单调增加的说法产生了怀疑。
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