Metallicities of M Dwarf Planet Hosts from Spectral Synthesis
Metallicities of M Dwarf Planet Hosts from Spectral Synthesis
复制标题
M 矮行星主星的光谱合成金属量
DOI：
10.1086/510527
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发表时间：
2006
期刊：
影响因子：
--
通讯作者：
M. Endl
中科院分区：
文献类型：
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作者：
Jacob L. Bean;G. F. Benedict;M. Endl
我们提出的第一光谱金属丰度的三个M矮星已知或候选行星质量的同伴。我们分析了这些恒星的高分辨率，高信噪比的光谱，我们在麦克唐纳天文台获得。我们的分析技术是基于最近修订的冷星模型大气和光谱合成代码的原子和分子特征的光谱合成。该技术已被证明产生的结果与太阳型恒星的分析一致，并允许测量M矮[M/H]值到0.12 dex精度。根据我们的分析，我们发现GJ 876、GJ 436和GJ 581的[M/H]分别=-0.12、-0.32和-0.33。这三颗M型矮行星的母星都有太阳下的金属丰度，这与FGK型恒星中观察到的趋势有着惊人的偏离。这项研究是我们正在进行的工作的第一部分，以确定麦克唐纳天文台行星搜索计划中包括的M矮星的金属丰度。
We present the first spectroscopic metallicities of three M dwarfs with known or candidate planetary mass companions. We have analyzed high-resolution, high signal-to-noise ratio spectra of these stars, which we obtained at McDonald Observatory. Our analysis technique is based on spectral synthesis of atomic and molecular features using recently revised cool-star model atmospheres and spectrum synthesis code. The technique has been shown to yield results consistent with the analyses of solar-type stars and allows measurements of M dwarf [M/H] values to 0.12 dex precision. From our analysis, we find [M/H] = -0.12, -0.32, and -0.33 for GJ 876, GJ 436, and GJ 581, respectively. These three M dwarf planet hosts have subsolar metallicities, a surprising departure from the trend observed in FGK-type stars. This study is the first part of our ongoing work to determine the metallicities of the M dwarfs included in the McDonald Observatory planet search program.