SILICON ABUNDANCES IN NEARBY STARS FROM THE Si i INFRARED LINES
SILICON ABUNDANCES IN NEARBY STARS FROM THE Si i INFRARED LINES
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DOI：
10.1088/0004-637x/755/1/36
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发表时间：
2012-07
期刊：
影响因子：
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通讯作者：
Jian-rong Shi;M. Takada-Hidai;Y. Takeda;K. Tan;Shaoming Hu;Gang Zhao;Chen Cao
中科院分区：
文献类型：
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作者：
Jian-rong Shi;M. Takada-Hidai;Y. Takeda;K. Tan;Shaoming Hu;Gang Zhao;Chen Cao
我们使用了来自莫纳克亚山顶的斯巴鲁望远镜的高分辨率、高信噪比的红外光谱。给出了近星大气中Si-I红外线的线形计算。[Si/Fe]的所有丰度结果都是从局域热力学平衡(LTE)和NLTE统计平衡计算和光谱合成方法得到的。我们发现，即使对于富含金属的恒星(>；0.1dex)，Si i红外线的NLTE效应也是重要的，并且NLTE效应可能取决于表面引力。当考虑NLTE效应时，光谱线和红外线的硅丰度得到了很好的一致，而LTE的结果却有很大的差异。对于金属贫乏的恒星来说，衍生出的硅丰度过高。
We have used high-resolution, high signal-to-noise ratio infrared spectra from the Subaru Telescope atop Mauna Kea. Line formation calculations of Si i infrared lines in the atmospheres of nearby stars are presented. All abundance results of [Si/Fe] are derived from local thermodynamic equilibrium (LTE) and NLTE statistical equilibrium calculations and spectrum synthesis methods. We found that NLTE effects for Si i infrared lines are important even for metal-rich stars (>0.1 dex), and the NLTE effects may depend on the surface gravities. A good agreement of silicon abundances between the optical and infrared lines is obtained when the NLTE effects are included, while a large difference is found for the LTE results. The derived silicon abundances are overabundant for metal-poor stars.