B-型变星复杂星震学对不透明度的限制：$β$造父星$θ$蛇夫座
Constraints on opacities from complex asteroseismology of B-type pulsators: the $β$ Cephei star $θ$ Ophiuchi
摘要：
我们提出了一个{ \bf全面}的$β$造父变星$θ$蛇夫座的星震建模的结果。{ \bf我们称这些研究为{ \it复杂星震学}，因为我们的目标是再现脉动频率以及由辐射通量扰动定义的复杂非绝热参数$f$的相应值。}为此，我们应用的方法，同时确定的球谐度，$\ell$，激发脉动模式和相应的非绝热$f$参数从组合多色测光和径向速度数据。使用OP和OPAL不透明度数据，我们发现一个家庭的地震模型，再现径向和偶极子质心模式频率，以及与径向模式相关的$f$参数。在B型主序星的地震模拟中加入非绝热参数，对恒星不透明度产生了很强的约束。特别是，只有一个来源的不透明度，它是可能的，同意的经验值$f$与他们的理论对应。我们对$θ$ Oph的结果基本上倾向于OPAL数据。
英文摘要：
We present results of a {\bf comprehensive} asteroseismic modelling of the $β$ Cephei variable $θ$ Ophiuchi. {\bf We call these studies {\it complex asteroseismology} because our goal is to reproduce both pulsational frequencies as well as corresponding values of a complex, nonadiabatic parameter, $f$, defined by the radiative flux perturbation.} To this end, we apply the method of simultaneous determination of the spherical harmonic degree, $\ell$, of excited pulsational mode and the corresponding nonadiabatic $f$ parameter from combined multicolour photometry and radial velocity data. Using both the OP and OPAL opacity data, we find a family of seismic models which reproduce the radial and dipole centroid mode frequencies, as well as the $f$ parameter associated with the radial mode. Adding the nonadiabatic parameter to seismic modelling of the B-type main sequence pulsators yields very strong constraints on stellar opacities. In particular, only with one source of opacities it is possible to agree the empirical values of $f$ with their theoretical counterparts. Our results for $θ$ Oph point substantially to preference for the OPAL data.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
