基于$\varepsilon$机制的III大质量主序星的振动不稳定性
Vibrational instability of Population III very massive main-sequence stars due to the $\varepsilon$-mechanism
摘要：
超大质量恒星被认为是在早期宇宙中形成的，因为缺乏重元素的冷却过程，并且可能是宇宙后来演化的原因。我们对它们演化的振动稳定性很感兴趣，并使用$500-3000M_{\sun}$对星族III超大质量主序星的径向和非径向振荡进行了线性非绝热分析。我们发现，只有径向基模变得不稳定，由于$\varepsilon$ -机制，这些恒星。这种不稳定性出现在CNO循环被激活，核能产生率大到足以停止主序前收缩之后，并在堆芯氢燃烧的早期阶段继续存在。此外，我们还粗略地估算了由于不稳定性而引起的质量损失量，以了解其重要性。
英文摘要：
Very massive stars are thought to be formed in the early Universe because of a lack of cooling process by heavy elements, and might have been responsible for the later evolution of the Universe. We had an interest in vibrational stability of their evolution and carried out the linear nonadiabatic analysis of radial and nonradial oscillations for population III very massive main-sequence stars with $500-3000M_{\sun}$. We found that only the radial fundamental mode becomes unstable due to the $\varepsilon$-mechanism for these stars. The instability appears just after the CNO cycle is activated and the nuclear energy generation rate becomes large enough to stop the pre--main-sequence contraction, and continues during the early stage of the core hydrogen burning. Besides, we roughly estimated amount of mass loss due to the instability to know its significance.
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