论文标题
B型超级$κ$ cassiopeiae模型中的不稳定性和脉动（HD 2905）
Instabilities and pulsations in models of the B-type supergiant $κ$ Cassiopeiae (HD 2905)
论文作者
论文摘要
对于B型超级$κ$ cassiopeiae（HD 2905）的变化，已经观察到数小时至几天之间的周期，从光图和光谱上观察到。 Simón-D \'ıaz等人对这颗星星的最新研究。 （2018年）揭示了可变性，主要期限为2.7天。为了了解这种可变性，我们就$κ$ cassiopeiae模型的径向扰动提出了线性的非绝热稳定性分析。与基本模式相关的不稳定性和第一个泛音是针对质量在27 m $ _ {\ odot} $和44 m $ _ {\ odot} $之间的模型的标识。对于选定的模型，通过数值模拟遵循不稳定性进入非线性制度。结果，发现有限振幅脉动，周期为3至1.8天。质量为34.5 m $ _ {\ odot} $的模型表现出与观测值一致的2.7天的脉动周期。在非线性政权中，不稳定性可能会导致信封的大量通胀。
For the B-type supergiant $κ$ Cassiopeiae (HD 2905) variabilities with periods between several hours and a few days have been observed both photometrically and spectroscopically. A recent study of this star by Simón-D\'ıaz et al. (2018) has revealed variability with a dominant period of 2.7 days. To understand this variability, we present a linear non-adiabatic stability analysis with respect to radial perturbations for models of $κ$ Cassiopeiae. Instabilities associated with the fundamental mode and the first overtone are identified for models with masses between 27 M$_{\odot}$ and 44 M$_{\odot}$. For selected models, the instabilities are followed into the non-linear regime by numerical simulations. As a result, finite amplitude pulsations with periods between 3 and 1.8 days are found. The model with a mass of 34.5 M$_{\odot}$ exhibits a pulsation period of 2.7 days consistent with the observations. In the non-linear regime, the instabilities may cause a substantial inflation of the envelope.
