论文标题
内部旋转和浮力旅行时间为60伽玛多拉德斯星星，来自不间断的苔丝光曲线，跨越352天
Internal rotation and buoyancy travel time of 60 gamma Doradus stars from uninterrupted TESS light curves spanning 352 days
论文作者
论文摘要
语境。伽马多拉德斯（以下称$γ$ 〜dor）是重力模式脉动器，其周期具有有关恒星内部结构的信息。这些时期对内部旋转和化学混合特别敏感，这两个过程在恒星进化理论中尚未得到很好的约束。目标。我们旨在确定脉动模式，并以106 $γ$ dor星星的形式推断出内部旋转和浮力旅行时间，该星星在其南部连续观看区域（以下S-CVZ）中观察到的超级球星调查卫星（TESS）任务（TESS）任务。我们依靠140个先前检测到的周期间距模式，即（近）连续的脉动模式周期。方法。我们使用渐近表达来计算旋转率和浮力行进时间范围的重力模式频率，这些频率覆盖了$γ$ 〜DOR恒星的物理范围。这些频率通过最小化自定义成本函数而适合观察到的周期间隔模式。使用传统的旋转近似值，使用恒星脉动代码Gyre评估了旋转的效果。结果。我们获得了60澳元$γ$ 〜DOR星的脉动模式识别，内部旋转和浮力旅行时间。对于其余46个目标，检测到的模式太短或包含太多缺失模式，无法进行明确的模式识别，并且需要更长的光曲线。对于成功分析的恒星，我们发现，从1年长的苔丝光曲线中的周期间隔模式可以将内部旋转和浮力旅行时间限制为分别为$ \ rm 0.03〜 d^{ - 1} $和400s和400s的精确度，这是基于4-幼二元的$ kepler Light curves $ culves $γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$γ$。
Context. Gamma Doradus (hereafter $γ$~Dor) stars are gravity-mode pulsators whose periods carry information about the internal structure of the star. These periods are especially sensitive to the internal rotation and chemical mixing, two processes that are currently not well constrained in the theory of stellar evolution. Aims. We aim to identify the pulsation modes and deduce the internal rotation and buoyancy travel time for 106 $γ$ Dor stars observed by the Transiting Exoplanet Survey Satellite (TESS) mission in its southern continuous viewing zone (hereafter S-CVZ). We rely on 140 previously detected period-spacing patterns, that is, series of (near-)consecutive pulsation mode periods. Methods. We used the asymptotic expression to compute gravity-mode frequencies for ranges of the rotation rate and buoyancy travel time that cover the physical range in $γ$~Dor stars. Those frequencies were fitted to the observed period-spacing patterns by minimising a custom cost function. The effects of rotation were evaluated using the traditional approximation of rotation, using the stellar pulsation code GYRE. Results. We obtained the pulsation mode identification, internal rotation and buoyancy travel time for 60 TESS $γ$~Dor stars. For the remaining 46 targets, the detected patterns are either too short or contained too many missing modes for unambiguous mode identification, and longer light curves are required. For the successfully analysed stars, we found that period-spacing patterns from 1-yr long TESS light curves can constrain the internal rotation and buoyancy travel time to a precision of $\rm 0.03~d^{-1}$ and 400s, respectively, which is about half as precise as literature results based on 4-yr Kepler light curves of $γ$~Dor stars.
