http://arxiv.org/abs/1802.01495
Variability and mass-loss are common phenomena in massive OB-type stars. It is argued that they are caused by violent strange mode instabilities identified in corresponding stellar models. We present a systematic linear stability analysis with respect to radial perturbations of massive OB-type stars with solar chemical composition and masses between 23 to 100 M${\odot}$. For selected unstable stellar models, we perform non-linear simulations of the evolution of the instabilities into the non-linear regime. Finite amplitude pulsations with periods in the range between hours and 100 days are found to be the final result of the instabilities. The pulsations are associated with a mean acoustic luminosity which can be the origin of a pulsationally driven wind. Corresponding mass-loss rates lie in the range between 10$^{-9}$ and 10$^{-4}$ M${\odot}$ yr$^{-1}$ and may thus affect the evolution of massive stars.
A. Yadav and W. Glatzel
Tue, 6 Feb 18
22/62
Comments: 17 pages, 25 figures, Published in MNRAS
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