TESS 任务观测到的含 $\eta$ Cep 星的食双星的整体脉动特征
Ensemble pulsational characteristics of eclipsing binaries containing $β$ Cep stars observed by the TESS mission
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中文总结 AI 辅助
本研究分析 TESS 观测的 65 颗食双星中 $\eta$ Cep 星的脉动特征，结合星震学建模推导内部性质，发现多数系统准刚性旋转，脉动振幅与频率负相关，与轨道周期无关。
中文摘要 AI 辅助
食双星中的大质量脉动星提供了精确的、与模型无关的恒星参数，这些参数与星震学约束相结合，为大质量恒星内部性质和角动量输运提供了强有力的探针。本研究调查了食双星中 $\eta$ Cep 脉动星的脉动特征及其对结构和演化的影响。我们分析了食双星中 65 颗 $\eta$ Cep 星的样本，尽可能识别旋转分裂模式，并统计研究脉动性质对双星轨道参数的依赖性。我们使用 MESA 模型网格和相关的 StORM 脉动频率，以及一个在 $\eta$ Cep 不稳定区内追踪恒星年龄和旋转的星震学程序，推导了它们的内部性质。对 14 个表现出旋转模式分裂的系统推导了内部旋转速率。虽然对 HD 112485 初步推断存在较差自转，但除 CZ Vel 外，其他系统与准刚性旋转一致。通过详细的向前星震学建模，推导了 HD 112485 和 EK Cru 的地震和演化性质。HD 112485 是迄今进行星震学建模的演化程度最低的 $\eta$ Cep 星之一，其核心氢质量分数 $X_{c}= 0.501_{-0.013}^{+0.009}$。HD 112485 中再现的两个纬向模式是第一个径向阶偶极压力模式和第二个径向阶四极重力模式，而 EK Cru 中的纬向模式是二阶四极混合模式和第三阶偶极压力模式。多元回归显示脉动振幅与脉动频率呈负相关，与轨道周期无统计学显著关系。此外，在该样本中，脉动频率与轨道周期之间未观察到显著关系。
英文摘要
Massive pulsators in eclipsing binaries provide precise, model-independent stellar parameters that, combined with asteroseismic constraints, provide powerful probes of interior properties and angular-momentum transport in massive stars. This study investigates the pulsational characteristics and their impact on the structure and evolution of $β$ Cep pulsators in eclipsing binaries. We analyse an ensemble of 65 $β$ Cep stars in eclipsing binaries, identify rotationally split modes where possible, and statistically investigate the dependence of pulsational properties on binary orbital parameters. We derive their interior properties using MESA model grids and associated StORM pulsation frequencies, together with an asteroseismic routine that tracks stellar age and rotation across the $β$ Cep instability region. Interior rotation rates are derived for 14 systems that exhibit rotational mode splitting. While differential rotation is tentatively inferred for HD 112485, the other systems, except CZ Vel, are consistent with quasi-rigid rotation. The seismic and evolutionary properties of HD 112485 and EK Cru are derived through detailed forward asteroseismic modelling. HD 112485 is one of the least evolved $β$ Cep stars asteroseismically modelled to date, with a core hydrogen mass fraction $X_{c}= 0.501_{-0.013}^{+0.009}$. The two reproduced zonal modes in HD 112485 are the first radial-order dipole pressure mode and the second radial-order quadrupole gravity mode, while the zonal modes in EK Cru are the second-order quadrupole mixed mode and the third order dipole pressure mode. A multivariate regression shows a negative correlation of the pulsation amplitude with pulsation frequency, and no statistically significant relationship with the orbital period. In addition, no significant relationship is observed between the pulsation frequency and the orbital period in this sample.
发表机构
- University of Nigeria, Nsukka（尼日利亚恩苏卡大学）
- KU Leuven（荷语鲁汶大学）
- Newcastle University（纽卡斯尔大学）
- Radboud University Nijmegen（奈梅亨拉德堡德大学）
- Max Planck Institut für Astronomie（马克斯·普朗克天文学研究所）
- Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文中心）
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