恒星表面的空间分辨光谱学。IV。F、G和K星：超高分辨率的合成3D光谱
Spatially resolved spectroscopy across stellar surfaces. IV. F, G, & K-stars: Synthetic 3D spectra at hyper-high resolution
摘要：
高精度恒星分析需要流体动力学3D建模。这些模型预测了恒星盘面上谱线形状、不对称性和波长偏移的变化。对于测试模型在恒星以外的太阳，空间分辨观测是可行的，从差分光谱在系外行星过境，检索光谱的恒星表面部分，相继成为隐藏在后面的过境行星，如论文I，II和III。现在可以从3D模型中获得扩展光谱区域的合成高分辨率光谱。与其他从头算模拟类似，这些数据包含尚未专门建模的模式，但可能会在类似于大量观测的分析后显示出来。从T=3964- 6726 K的五个3D模型（约光谱类型K8 V-F3 V），分析超高分辨率（R> 1，000，000）的合成光谱。选定的FeI和FeII线在不同位置的恒星盘进行搜索模式之间的不同线在同一颗恒星和不同的恒星之间的类似的线。这种模式被确定为代表光球线的不同强度，激发电位，电离水平，编码的流体动力学的三维结构。线剖面和平分线显示了不同的恒星在不同位置的恒星盘。绝对对流波长的变化，获得作为差异的一维模型，在这种变化不会发生。从现实复杂的合成光谱中检索线属性的可观测关系。这种模式还可以测试非常详细的3D建模，包括非LTE效果。虽然目前的结果是在超高光谱分辨率下获得的，但随后的论文V在实际较低的分辨率和存在噪声的情况下研究了它们的实际可观测性。
英文摘要：
High-precision stellar analyses require hydrodynamic 3D modeling. Such models predict changes across stellar disks of spectral line shapes, asymmetries, and wavelength shifts. For testing models in stars other than the Sun, spatially resolved observations are feasible from differential spectroscopy during exoplanet transits, retrieving spectra of stellar surface segments that successively become hidden behind the transiting planet, as shown in Papers I, II, and III. Synthetic high-resolution spectra over extended spectral regions are now available from 3D models. Similar to other ab initio simulations, these data contain patterns that have not been specifically modeled but may be revealed after analyses analogous to those of a large volume of observations. From five 3D models spanning T=3964-6726K (approx. spectral types K8V-F3V), synthetic spectra at hyper-high resolution (R>1,000,000) were analyzed. Selected FeI and FeII lines at various positions across stellar disks were searched for patterns between different lines in the same star and for similar lines between different stars. Such patterns are identified for representative photospheric lines of different strengths, excitation potential, and ionization level, encoding the hydrodynamic 3D structure. Line profiles and bisectors are shown for various stars at different positions across stellar disks. Absolute convective wavelength shifts are obtained as differences to 1D models, where such shifts do not occur. Observable relationships for line properties are retrieved from realistically complex synthetic spectra. Such patterns may also test very detailed 3D modeling, including non-LTE effects. While present results are obtained at hyper-high spectral resolution, the subsequent Paper V examines their practical observability at realistically lower resolutions, and in the presence of noise.
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