Effect of chemical abundance on a Wolf-Rayet stellar wind driven by radiation pressure and Alfven waves

Details Effect of chemical abundance on a Wolf-Rayet stellar wind driven by radiation pressure and Alfven waves Effect of chemical abundance on a Wolf-Rayet stellar wind driven by radiation pressure and Alfven waves

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...270..345d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 270, no. 1-2, p. 345-354.

Astronomy and Astrophysics

Astrophysics

8

Chemical Composition, Magnetohydrodynamic Waves, Radiation Pressure, Stellar Winds, Wolf-Rayet Stars, Plasma Pressure, Stellar Composition, Stellar Mass Ejection

Scientific paper

Observations of early-type stars in the UV have shown that these stars lose a considerable part of their mass in the form of a stellar wind, which led to the development of a radiation-driven wind theory to explain the mass loss. In this model, momentum is transferred from the radiation field to the gas by the scattering of the radiation, principally by spectral lines. Radiation pressure models, however, are limited. The mass loss rates and the terminal velocities of Wolf-Rayet stars cannot be explained by these models; thus an alternative mechanism is considered. We investigate a model for Wolf-Rayet stars, where both a flux of Alfven waves and radiation pressure are important. The correction factor, which allows for the finite size of the stellar disk, is taken into account. The effect of chemical composition, as well as a truncated line spectrum, are investigated. We find that, whereas for a solar abundance atmosphere an average surface magnetic field of about 600 G is required, for a He atmosphere the minimum magnetic field is appreciably less.

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