M-矮星中FeH的Teff和logg依赖性
Teff and logg dependence of FeH in M-dwarfs
摘要：
本文给出了几个M矮星模型（logg=3.0-5.0 [cgs]，Teff= 2800 K-3450 K）在Z-滤波器范围内的合成FeH带谱。我们的目的是在M-矮星的对流速度的特点，并给出一个粗略的估计范围内，三维大气处理是必要的，其中一维大气模型足以解释分子光谱特征。这对于区分速度展宽和旋转展宽或塞曼展宽也很重要。使用3D CO 5 BOLD辐射流体动力学（RHD）模型和线合成代码LINFOR 3D计算合成光谱。我们使用完整的3D模型和高分辨率的3D光谱合成的详细研究一些孤立的FeH线。FeH线强度显示出对表面重力和有效温度的依赖性，并且可以用来测量M型物体中的这两个量。谱线宽度与模型星的速度场有关，而速度场强烈依赖于表面引力。此外，我们调查的速度场在三维M-矮星模型连同相关的微观和宏观湍流速度在一维的情况下。我们还搜索对线形的影响。
英文摘要：
We present synthetic FeH band spectra in the z-filter range for several M-dwarf models with logg=3.0-5.0 [cgs] and Teff=2800K -3450K. Our aim is to characterize convective velocities in M-dwarfs and to give a rough estimate of the range in which 3D-atmosphere treatment is necessary and where 1D-atmosphere models suffice for the interpretation of molecular spectral features. This is also important in order to distinguish between the velocity-broadening and the rotational- or Zeeman-broadening. The synthetic spectra were calculated using 3D CO5BOLD radiative-hydrodynamic (RHD) models and the line synthesis code LINFOR3D. We used complete 3D-models and high resolution 3D spectral synthesis for the detailed study of some well isolated FeH lines. The FeH line strength shows a dependence on surface gravity and effective temperature and could be employed to measure both quantities in M-type objects. The line width is related to the velocity-field in the model stars, which depends strongly on surface gravity. Furthermore, we investigate the velocity-field in the 3D M-dwarf models together with the related micro- and macro-turbulent velocities in the 1D case. We also search for effects on the lineshapes.
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