Spindown of massive rotating stars
arXiv:1103.5481 · doi:10.1111/j.1365-2966.2011.18766.x
Abstract
Models of rapidly rotating massive stars at low metallicities show significantly different evolution and higher metal yields compared to non-rotating stars. We estimate the spin-down time-scale of rapid rotating non-convective stars supporting an alpha-Omega dynamo. The magnetic dynamo gives rise to mass loss in a magnetically controlled stellar wind and hence stellar spin down owing to loss of angular momentum. The dynamo is maintained by strong horizontal rotation-driven turbulence which dominates over the Parker instability. We calculate the spin-down time-scale and find that it could be relatively short, a small fraction of the main-sequence lifetime. The spin-down time-scale decreases dramatically for higher surface rotations suggesting that rapid rotators may only exhibit such high surface velocities for a short time, only a small fraction of their main-sequence lifetime.
Accepted by MNRAS
References in corpus (5)
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Cited by in corpus (8)
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- A search for Galactic runaway stars using Gaia Data Release 1 and Hipparcos proper motions
- Towards a unified model of stellar rotation
- Critical angular velocity and anisotropic mass loss of rotating stars with radiation-driven winds
- Stellar Photospheric Abundances as a Probe of Disks and Planets
- Spindown of massive rotating stars
- Dynamics of the radiative envelope of rapidly rotating stars: Effects of spin-down driven by mass loss
- Multiverse Predictions for Habitability: Element Abundances