从具有$\langle 3\mathrm{D} \rangle$ -大气的恒星模型得到的太阳型矮星的理论振荡频率
Theoretical oscillation frequencies for solar-type dwarfs from stellar models with $\langle 3\mathrm{D} \rangle$-atmospheres
摘要：
我们提出了一种新的方法，用于替换恒星模型的最外层与内插大气的基础上从3D模拟的结果，以纠正这些层的结构不足。这种替换称为修补。测试，基于三个不同的代码和不同的输入物理内部模型的三维大气，进行。使用太阳能模型，我们研究不同的修补标准如何影响本征频率。这些标准包括执行替换的深度、替换所基于的数量以及未修补模型和修补3D大气之间的$T_\mathrm{eff}$和$\log g$的不匹配。我们发现本征频率是不变的修补深度内的绝热区域，而改变修补量或所采用的大气网格导致的频率偏移，可能会超过$1\,μ\mathrm{Hz}$。同样，本征频率对$T_\mathrm{eff}$或$\log g$中的失配敏感。一个新的计划，平均三维分层内插大气网格的精度进行了深入的调查。在大气网格的大部分地区，我们的插值方案产生足够准确的结果，为目的的asteroseismology。我们将我们的程序应用于四颗\textit{Kepler}恒星的星震分析，并得出与太阳情况相同的结论：结构缺陷的校正降低了本征频率，这种校正对修补标准稍微敏感，模型和观测之间的剩余频率差异与频率的依赖性较小。我们的工作显示了修补在星震学中的适用性和相关性。
英文摘要：
We present a new method for replacing the outermost layers of stellar models with interpolated atmospheres based on results from 3D simulations, in order to correct for structural inadequacies of these layers. This replacement is known as patching. Tests, based on 3D atmospheres from three different codes and interior models with different input physics, are performed. Using solar models, we investigate how different patching criteria affect the eigenfrequencies. These criteria include the depth, at which the replacement is performed, the quantity, on which the replacement is based, and the mismatch in $T_\mathrm{eff}$ and $\log g$ between the un-patched model and patched 3D atmosphere. We find the eigenfrequencies to be unaltered by the patching depth deep within the adiabatic region, while changing the patching quantity or the employed atmosphere grid leads to frequency shifts that may exceed $1\,μ\mathrm{Hz}$. Likewise, the eigenfrequencies are sensitive to mismatches in $T_\mathrm{eff}$ or $\log g$. A thorough investigation of the accuracy of a new scheme, for interpolating mean 3D stratifications within the atmosphere grids, is furthermore performed. Throughout large parts of the atmosphere grids, our interpolation scheme yields sufficiently accurate results for the purpose of asteroseismology. We apply our procedure in asteroseismic analyses of four \textit{Kepler} stars and draw the same conclusions as in the solar case: Correcting for structural deficiencies lowers the eigenfrequencies, this correction is slightly sensitive to the patching criteria, and the remaining frequency discrepancy between models and observations is less frequency-dependent. Our work shows the applicability and relevance of patching in asteroseismology.
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