Building Reliable Models of M Dwarf Chromospheres: The Spectral Diagnostics
Building Reliable Models of M Dwarf Chromospheres: The Spectral Diagnostics
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建立可靠的 M 矮星色球模型：光谱诊断
DOI：
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发表时间：
2000
期刊：
影响因子：
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通讯作者：
P. Mauas
中科院分区：
文献类型：
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作者：
P. Mauas
作为一项正在进行的研究半经验构建的色球模型拟合冷恒星色球光谱的可靠性的项目的一部分，本文研究了dM和dMe恒星的假设色球结构的变化如何影响发射光谱。通过这种方式，我们研究了一组给定的特征是否可以完全决定大气结构，推断出的大气参数中的不确定性有多大，以及计算出的大气模式在多大程度上可以被认为是唯一的。我们发现CaⅱK线或Na D线的谱线可以用来确定Tmin区域的结构，而Hα谱线可以提供色球结构的良好信息。Lyα通量，反过来，可以用来约束过渡区的位置。
As part of an ongoing project to study how reliable are the chromospheric models constructed semiempirically to fit the chromospheric spectrum of cold stars, in this paper we study how changes in the assumed chromospheric structure of dM and dMe stars affect the emitted spectrum. In this way, we study if a given set of features can wholly determine the atmospheric structure, how large are the indeterminations in the atmospheric parameters deduced, and to what extent the atmospheric model computed can be considered unique. We find that the profiles of the Ca II K line or the Na D lines can be used to determine the structure of the Tmin region and that the Hα profile can provide good information on the structure of the chromosphere. The Lyα flux, in turn, can be used to constrain the position of the transition region.