The nature of the Wolf-Rayet phenomenon: mass loss close to the Eddington limit

Details The nature of the Wolf-Rayet phenomenon: mass loss close to the Eddington limit The nature of the Wolf-Rayet phenomenon: mass loss close to the Eddington limit

Aug 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008rmxac..33...88g&link_type=abstract

Massive Stars: Fundamental Parameters and Circumstellar Interactions (Eds. P. Benaglia, G. L. Bosch, & C. E. Cappa) Revista Mexi

Astronomy and Astrophysics

Astronomy

Stars: Mass Loss, Stars: Winds, Outflows, Stars: Wolf-Rayet

Scientific paper

With the new Potsdam Wolf-Rayet (PoWR) hydrodynamic atmosphere models we have obtained the first fully self-consistent wind models for WR stars. We find that WR-type mass loss is initiated when stars approach the Eddington limit. For the most massive stars this happens already at the end of their main-sequence lifetime, i.e. still in the H-burning phase. Less massive objects enter the Wolf-Rayet stage after the onset of He-burning. From spectral analyses with hydrodynamic models we estimate the masses of two extremely luminous, H-rich WNL stars in Carina OB 1. With present masses of at least 80-100 M_&sun;, these stars are the direct descendants of the most massive stars in the galaxy.

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