Vibrational instability of Population III very massive main-sequence stars due to the $\epsilon$-mechanism

Abstract

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 $\epsilon$-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.

5 pages, 3 figures, accepted for publication in MNRAS Letters

References in corpus (3)

• Ultraluminous X-ray Sources in the Chandra and XMM-Newton Era
• Effects of rotation on the evolution of primordial stars
• Vibrational instability of Population III very massive main-sequence stars due to the $\epsilon$-mechanism

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• Pulsational instability of supergiant protostars: Do they grow supermassive by accretion?
• Pulsation-driven mass loss from massive stars behind stellar mergers in metal-poor dense clusters
• Vibrational instability of Population III very massive main-sequence stars due to the $\epsilon$-mechanism
• The Stability of Massive Main Sequence Stars as a Function of Metallicity