Mass loss from Wolf-Rayet stars due to radiation pressure and Alfven waves

Details Mass loss from Wolf-Rayet stars due to radiation pressure and Alfven waves Mass loss from Wolf-Rayet stars due to radiation pressure and Alfven waves

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...410..732d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 410, no. 2, p. 732-739.

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32

Plasma Waves, Radiation Pressure, Stellar Mass Ejection, Wolf-Rayet Stars, Computational Astrophysics, Equations Of Motion, Momentum Transfer, Stellar Magnetic Fields, Stellar Models

Scientific paper

We discuss the physical mechanism that can explain the observed large mass loss in luminous, Wolf-Rayet (WR) stars. Interpreted classically, the P Cygni line profiles imply that the terminal velocity of the flow is about 2500 km/s. These winds are generally interpreted as radiation pressure line-driven. Radiation pressure line-driven models, however, present difficulties in explaining several observational characteristics of these stars. We investigate, in particular, the disagreement between the observational mass-loss rates in WR stars and the maximum predicted mass loss by radiation pressure. We investigate a model for mass-loss rates from WR stars, where both a flux of Alfven waves and radiation pressure are important in order to reproduce the terminal velocity observed. Our model is a fusion of the Alfven wave wind model of Jatenco-Pereira and Opher and the radiation pressure model of Castor et al. (1975). Whereas a pure Alfven wave-driven model requires a magnetic field of about 20,000 G, in our model we find that the required magnetic field is less than 1000 G.

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