论文标题
苔丝A和B星和Maia变量之间的脉动
Pulsation among TESS A and B stars and the Maia variables
论文作者
论文摘要
在1-18的部门中，超过50000个苔丝星的分类导致检测到766个脉动主序列B星以及超过5000 $δ$ SCUTI，2300 $γ$ Doradus和114个ROAP候选者。发现不存在一组独特的$β$ cephei恒星，该恒星被定义为频率大于2.5 d $^{ - 1} $并通过模型预测的B星。取而代之的是，将在整个B-Star系列中找到高频，最终与$δ$ Scuti星星合并。高频脉动的酷B星是Maia变量。结果表明，Maia变量不是快速旋转的$β$ CEPHEI或SPB星。在发现$β$ Cephei变量的区域中，脉动恒星的比例较大，幅度较高，并且在单个模式下以较低的旋转速率在脉动中相当大。没有独特的SPB不稳定性区域。在所有B恒星中都发现了低频中的恒星脉动鞋底。最多，只有三分之一的B恒星似乎是脉动的。这些结果以及大部分A和B恒星显示旋转调制的事实表明，需要修改有关带有辐射信封的恒星的当前思想。
Classification of over 50000 TESS stars in sectors 1-18 has resulted in the detection of 766 pulsating main sequence B stars as well as over 5000 $δ$ Scuti, 2300 $γ$ Doradus and 114 roAp candidates. It is found that a distinct group of $β$ Cephei stars, defined as B stars with frequencies greater than 2.5 d$^{-1}$ and predicted by models, does not exist. Instead, high frequencies are to be found over the whole B-star range, eventually merging with $δ$ Scuti stars. The cool B stars pulsating in high frequencies are the Maia variables. It is shown that Maia variables are not rapidly-rotating $β$ Cephei or SPB stars. In the region where $β$ Cephei variables are found, the proportion of pulsating stars is larger and amplitudes are higher and a considerable fraction pulsate in a single mode and low rotation rate. There is no distinct SPB instability region. Stars pulsating sole in low frequencies are found among all B stars. At most, only one-third of B stars appear to pulsate. These results, as well as the fact that a large fraction of A and B stars show rotational modulation, indicate a need for a revision of current ideas regarding stars with radiative envelopes.
