Fully Nonadiabatic Analysis of Vibrational Instability of Population III Stars due to the $\epsilon$-Mechanism

Abstract

A linear nonadiabatic analysis of the vibrational stability of population III main-sequence stars was carried out. It was demonstrated that, in the case of massive stars with $M \gtrsim 5\Mo$, helium burning (triple alpha reaction) starts during the main-sequence stage and produces ${}^{12}\mathrm{C}$, leading to the activation of a part of the CNO-cycle. It was found that, despite of that, those stars with $M\lesssim 13\Mo$ become unstable against the dipole g${}_1$- and g${}_2$-modes due to the $\epsilon$-mechanism, during the early evolutionary phase at which the pp-chain is still the dominant nuclear energy source. The instability due to the $\epsilon$-mechanism occurs against g-modes having a large amplitude in the off-centered ${}^3$He accumulation shell in the deep interior, and the growth time is much shorter than the evolutionary timescale. This instability is therefore likely to induce mixing in the stellar interior, and have a significant influence on the evolution of these stars.

PASJ, 64, 2 (2012) in press. 9 pages, 8 figures

References in corpus (1)

• Modules for Experiments in Stellar Astrophysics (MESA)

Cited by in corpus (5)

• The Stability of Massive Main Sequence Stars as a Function of Metallicity
• Dipole low-order g mode instability of metal-poor low-mass main-sequence stars due to the $\epsilon$-mechanism
• Stability Analysis of Strange-Modes in Hot Massive Stars with Time-Dependent Convection
• Analysis of strange-mode instability with time-dependent convection in hot massive stars
• Vibrational Instability of Metal-Poor Low-Mass Main-Sequence Stars