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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Elemental abundances of M dwarfs based on high-resolution near-infrared spectra: Verification by binary systems
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Elemental abundances of M dwarfs based on high-resolution near-infrared spectra: Verification by binary systems

机译：基于高分辨率近红外光谱的M个矮星的元素丰富：二元系统验证

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摘要

M dwarfs are prominent targets of planet search projects, and their chemical composition is crucial to understanding the formation process or interior of orbiting exoplanets. However, measurements of elemental abundances of M dwarfs have been limited due to difficulties in the analysis of their optical spectra. We conducted a detailed chemical analysis of five M dwarfs (T-eff similar to 3200-3800 K), which form binary systems with G/K-type stars, by performing a line-by-line analysis based on high-resolution (R similar to 80000) near-infrared (960-1710 nm) spectra obtained with CARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Echelle Spectrographs). We determined the chemical abundances of eight elements (Na, Mg, K, Ca, Ti, Cr, Mn, and Fe), which are in agreement with those of the primary stars within measurement errors (similar to 0.2 dex). Through the analysis process, we investigated the unique behavior of atomic lines in a cool atmosphere. Most atomic lines are sensitive to changes in the abundance of not only the corresponding elements but also other elements, especially dominant electron donors such as Na and Ca. The Ti I lines show a negative correlation with the overall metallicity at T-eff < 3400 K due to the consumption of neutral titanium by the formation of TiO molecules. These findings indicate that to estimate the overall metallicity or the abundance of any element correctly, we need to determine the abundances of other individual elements consistently.
机译：矮星是行星搜索项目的主要目标，它们的化学成分对于理解绕轨道运行的系外行星的形成过程或内部至关重要。然而，由于光谱分析的困难，M矮星元素丰度的测量一直受到限制。我们对五颗M矮星（T-eff类似于3200-3800 K）进行了详细的化学分析，它们与G/K型恒星形成了双星系统，通过基于CARMENES获得的高分辨率（R类似于80000）近红外（960-1710 nm）光谱进行逐行分析（Calar Alto使用近红外和光学Echelle光谱仪对具有外地球的M矮星进行高分辨率搜索）。我们测定了八种元素（Na、Mg、K、Ca、Ti、Cr、Mn和Fe）的化学丰度，这些元素在测量误差范围内（类似于0.2 dex）与主星的化学丰度一致。通过分析过程，我们研究了原子线在冷空气中的独特行为。大多数原子线不仅对相应元素的丰度变化敏感，而且对其他元素的丰度变化也敏感，尤其是主要电子供体，如Na和Ca。由于TiO分子的形成消耗了中性钛，Ti I线在T-eff<3400 K时与整体金属丰度呈负相关。这些发现表明，要正确估计任何元素的总体金属丰度或丰度，我们需要一致地确定其他单个元素的丰度。

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