KIC 10526294：一颗缓慢旋转的B星，具有旋转分裂，准等间距重力模式
KIC 10526294: a slowly rotating B star with rotationally split, quasi-equally spaced gravity modes
摘要：
大质量恒星对于宇宙的化学富集非常重要。由于内部混合过程影响它们的寿命，因此对它们的核过冲和内部自转轮廓等物理参数进行约束，从而校正它们的恒星结构和演化模型是非常重要的。虽然迄今为止，已经证明星震学能够提供最精确的限制，但提供定量结果的详细地震研究的数量有限。我们的目标是通过深入的案例研究来扩展这一有限的样本，并提供一组约束良好的asteroseismic参数，为正在进行的β Cep和SPB恒星不稳定带的测绘工作做出贡献。我们推导出的基本参数，从高分辨率光谱，光谱合成技术。我们使用自定义掩模从开普勒卫星的原始像素级数据中获得最佳光变曲线。我们使用标准的时间序列分析工具来构建一组重要的脉动模式，为之后进行的地震分析提供基础。我们发现KIC 10526294是一颗冷的SPB星，是迄今为止发现的旋转速度最慢的恒星之一，尽管如此，开普勒观测的长度足以分辨出它的19个准等间距偶极模中的每一个的窄旋转分裂多重态。在这个系列中检测到的连续（径向顺序）偶极模式的数量比以往任何时候都高。所观察到的分裂量显示出一个增加的趋势，朝着更长的周期，这在很大程度上独立于地震校准的恒星模型指向一个非刚性的内部旋转配置文件。从平均分裂我们推断旋转周期约为188 d。从地震模型中，我们发现这颗恒星是年轻的，中心氢质量分数X_c> 0.64;它有一个超过α_ov <= 0.15的核心。
英文摘要：
Massive stars are important for the chemical enrichment of the universe. Since internal mixing processes influence their lives, it is very important to place constraints on the corresponding physical parameters, such as core overshooting and the internal rotation profile, so as to calibrate their stellar structure and evolution models. Although asteroseismology has been shown to be able to deliver the most precise constraints so far, the number of detailed seismic studies delivering quantitative results is limited. Our goal is to extend this limited sample with an in-depth case study and provide a well-constrained set of asteroseismic parameters, contributing to the ongoing mapping efforts of the instability strips of the beta Cep and SPB stars. We derived fundamental parameters from high-resolution spectra using spectral synthesis techniques. We used custom masks to obtain optimal light curves from the original pixel level data from the Kepler satellite. We used standard time-series analysis tools to construct a set of significant pulsation modes that provide the basis for the seismic analysis carried out afterwards. We find that KIC 10526294 is a cool SPB star, one of the slowest rotators ever found. Despite this, the length of Kepler observations is sufficient to resolve narrow rotationally split multiplets for each of its 19 quasi-equally spaced dipole modes. The number of detected consecutive (in radial order) dipole modes in this series is higher than ever before. The observed amount of splitting shows an increasing trend towards longer periods, which - largely independent of the seismically calibrated stellar models - points towards a non-rigid internal rotation profile. From the average splitting we deduce a rotation period of ~188 d. From seismic modelling, we find that the star is young with a central hydrogen mass fraction X_c>0.64; it has a core overshooting alpha_ov<=0.15.
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