从开普勒任务描述空间测光时代δ Sct星的观测特性
Characterising the observational properties of δ Sct stars in the era of space photometry from the Kepler mission
摘要：
δ Sct星是一组不同的中等质量脉动星，位于赫罗图中经典不稳定带的主序星上或附近。这些恒星中有许多是混合恒星，它们同时以压力和重力模式脉动，探测恒星内部不同深度的物理现象。利用开普勒空间望远镜观测到的两个大的δ Sct星群，研究了开普勒任务数据固有的仪器偏差和这些恒星的统计特性。这项工作的一个重要重点是分析脉动和恒星参数之间的关系，以及它们在经典不稳定带内的分布。研究发现，在经典不稳定边界的理论预测之外，存在着不可忽略的一部分主序星，这表明在Hertzsprung-Russell图中，需要一个依赖于质量的混合长度参数来同时解释δ Sct星的低径向阶和高径向阶压力模.此外，搜索的振幅谱的这些恒星，特别是连续的径向顺序的压力模式之间的频率差。在这项工作中，它被证明，一个基于集合的方法，使用空间测光从开普勒任务不仅是合理的δ Sct星，但它是一个有价值的方法，以确定最有前途的恒星模式识别和asteroseismic建模。研究δ Sct恒星的全部科学潜力尚未实现。本文中讨论的合奏代表了一个高质量的数据集，为未来的研究旋转和角动量输运内A和F星使用asteroseismology。
英文摘要：
The δ Sct stars are a diverse group of intermediate-mass pulsating stars located on and near the main sequence within the classical instability strip in the Hertzsprung-Russell diagram. Many of these stars are hybrid stars pulsating simultaneously with pressure and gravity modes that probe the physics at different depths within a star's interior. Using two large ensembles of δ Sct stars observed by the Kepler Space Telescope, the instrumental biases inherent to Kepler mission data and the statistical properties of these stars are investigated. An important focus of this work is an analysis of the relationships between the pulsational and stellar parameters, and their distribution within the classical instability strip. It is found that a non-negligible fraction of main sequence δ Sct stars exist outside theoretical predictions of the classical instability boundaries, which indicates the necessity of a mass-dependent mixing length parameter to simultaneously explain low- and high-radial order pressure modes in δ Sct stars within the Hertzsprung-Russell diagram. Furthermore, a search for regularities in the amplitude spectra of these stars is also presented, specifically the frequency difference between pressure modes of consecutive radial order. In this work, it is demonstrated that an ensemble-based approach using space photometry from the Kepler mission is not only plausible for δ Sct stars, but that it is a valuable method for identifying the most promising stars for mode identification and asteroseismic modelling. The full scientific potential of studying δ Sct stars is as yet unrealised. The ensembles discussed in this paper represent a high-quality data set for future studies of rotation and angular momentum transport inside A and F stars using asteroseismology.
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