Self-consistent models of Wolf-Rayet stars as helium stars with optically thick winds

Details Self-consistent models of Wolf-Rayet stars as helium stars with optically thick winds Self-consistent models of Wolf-Rayet stars as helium stars with optically thick winds

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...394..305k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 394, no. 1, July 20, 1992, p. 305-312.

Astronomy and Astrophysics

Astrophysics

44

Stellar Models, Stellar Winds, Wolf-Rayet Stars, Helium, Hertzsprung-Russell Diagram, Optical Thickness, Photosphere, Stellar Cores, Stellar Envelopes

Scientific paper

A helium star with a steady, optically thick wind is proposed as a first-order model for Wolf-Rayet stars. Using an enhanced opacity which is guided by results of recent opacity calculations, self-consistent solutions are obtained which are made up of an inner helium-burning core in hydrostatic equilibrium and an outer radiative envelope through which a steady state wind is accelerated. The surface is at optical depth near unity. The models are of homogeneous composition (primarily helium) and are of mass in the range 9-30 solar masses. In the most massive model, the momentum of the mass flow exceeds the photon momentum at the photosphere by a factor of 30. Terminal wind velocities are of order 1000 km/s; these velocities are lower limits, as we neglect line-driven wind acceleration above the photosphere. For an appropriate choice of the opacity enhancement law, models of different mass define a relationship between the mass-loss rate and the photospheric temperature which is consistent with observed data. A forbidden region is found in the low-temperature part of the H-R diagram where no thick wind solutions exist.

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