On the Eddington limit and WR Stars

Details On the Eddington limit and WR Stars On the Eddington limit and WR Stars

2012-01-24

arxiv.org/abs/1201.5013v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Accepted for publication in A&A, 7 pages, 6 figures

Scientific paper

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.

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