Radiatively driven winds in Wolf-Rayet stars - A unified core-atmosphere model

Statistics – Computation

Scientific paper

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Stellar Atmospheres, Stellar Cores, Stellar Models, Stellar Winds, Wolf-Rayet Stars, Computational Astrophysics, Dynamic Models, Stellar Envelopes, Stellar Mass, Stellar Mass Ejection

Scientific paper

A sequence of chemically homogeneous, dynamical stellar models is constructed for different masses. Each model is computed by fitting onto a helium-burning core a dynamical optically thick radiative envelope and an expanding atmosphere in which line acceleration is taken into account. The fitting procedure uniquely determines all the properties of the configuration, including the mass-loss rate M(dot) and the terminal velocity v(infinity), as a function of the total mass M. Although the bulk of the acceleration takes place in the atmosphere and is mainly due to line driving, dynamics is found to be not completely negligible even below the thermalization radius where only the gradients of isotropic radiation and gas pressure are responsible for acceleration. The derived values of M(dot) and v(infinity) are in good agreement with the observational data for Wolf-Rayet stars. In particular, the M(dot) versus M relation derived by Abbott et al. (1986) for W-R stars in binary systems is well reproduced.

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