On the Eddington limit and WR Stars
arXiv:1201.5013 · doi:10.1051/0004-6361/201118328
Abstract
We examine some properties of stars evolving close to the classical Eddington limit for electron-scattering opacity, when these stars maintain a chemically homogeneous structure as a result of mixing and/or mass loss. We consider analytical relations and models computed with the Geneva code. Homologous, chemically homogeneous stars evolving with a constant Eddington factor obey a relation of the form mu^2 M = const. This applies, for example, to Wolf-Rayet (WR) stars in stages without hydrogen. The value of the constant may depend on the metallicity, initial mass, evolutionary stage, and physical processes included in the considered homologous evolutionary sequence. An average value of the constant between 20 and 40 in solar units is consistent with the masses of Galactic WR stars.
Accepted for publication in A&A, 7 pages, 6 figures
References in corpus (5)
- Grids of stellar models with rotation - I. Models from 0.8 to 120 Msun at solar metallicity (Z = 0.014)
- Physical Properties of Wolf-Rayet Stars
- The Galactic WN stars: Spectral analyses with line-blanketed model atmospheres versus stellar evolution models with and without rotation
- The evolution of runaway stellar collision products
- Maximum stellar mass versus cluster membership number revisited
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