论文标题
在红色巨星中，结构变化对渐近混合模式耦合因子的贡献
Contributions of structural variations to the asymptotic mixed-mode coupling Factor in red giant stars
论文作者
论文摘要
超精致光度法任务的出现使得可以使用混合模式调查恒星内部的可能性。在第一个疏水器期间留下的化学成分的不连续性引起的结构变化 - UP是位于恒星中层的重要特征，该特征位于燃油燃烧的壳和红色巨人对流区之间的恒星中层，因为混合模性能可能会受到这些变化的重大影响。在本文中，使用出色的模型讨论了混合模式耦合因子$ Q $的变化的因素。通常，结构变化会导致羔羊频率的细微位移和浮力频率的急剧变化，从而导致使用渐近形式主义计算出的$ q $的变化，这些形式上假设具有平稳的背景没有结构变化。在低亮度红色巨人中，可以在可检测的混合模式中感受到这两个因素的影响。此外，两个特征频率的变化的不同性质在对流区域的底部附近有半径，在进化的红色巨人中会突然增加$ q $。随后，随着恒星沿着红色巨人分支进一步发展，这是快速下降的$ q $。
The advent of ultra-precise photometry space missions enable the possibility of investigating stellar interior with mixed modes. The structural variations induced by the discontinuity of the chemical composition left behind during the first dredge--up is an important feature in the stellar mid-layers located between the hydrogen-burning shell and the base of the convective zone of red giants, as the mixed-mode properties can be significantly affected by these variations. In this paper, the contributing factors to variations of the mixed-mode coupling factor, $q$, are discussed with stellar models. In general, the structural variations give rise to a subtle displacement in the Lamb frequency and a sharp change in the buoyancy frequency, which lead to variations in the value of $q$ computed using the asymptotic formalisms that assuming a smooth background free of structural variations. The impact of these two factors can be felt in detectable mixed modes in low-luminosity red giants. Furthermore, the different nature of variations of the two characteristic frequencies with radius near the base of the convective zone, produces a sudden increase in $q$ in evolved red giants. This is followed by a quick drop in $q$ as the star evolves further along the red giant branch.
