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Dynamics and variability of winds from single Wolf-Rayet stars

Published online by Cambridge University Press:  25 May 2016

Stanley P. Owocki  and
Kenneth G. Gayley
Stanley P. Owocki
Affiliation:
Bartol Research Institute, University of Delaware, Newark, DE 19350, USA
Kenneth G. Gayley
Affiliation:
Department of Physics and Astronomy, University of Iowa, Iowa City, IA 52245, USA

Abstract

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We review the dynamics of winds from single Wolf-Rayet stars, with emphasis on the following specific points:

  1. (a) The classical “momentum problem” (to explain the large inferred ratio of wind to radiative momentum, η Mv∞/(L/c) ≫ 1) is in principle readily solved through multiple scattering of radiation by an opacity that is sufficiently “gray” in its spectral distribution. In this case, one simply obtains η ≃ τ, where τ is the wind optical depth;

  2. (b) Lines with a Poisson spectral distribution yield an “effectively gray” cumulative opacity, with multi-line scattering occuring when the velocity separation between thick lines Δv is less than the wind terminal speed v∞. In this case, one obtains η ≃ v∞/Δv;

  3. (c) However, realistic line lists are not gray, and leakage through gaps in the line spectral distribution tends to limit the effective scattering to η ≲ 1;

  4. (d) In WR winds, ionization stratification helps spread line-bunches and so fill in gaps, allowing for more effective global trapping of radiation, and thus η > 1;

  5. (e) However, photon thermalization can reduce the local effectiveness of line-driving near the stellar core, making it difficult for radiation alone to initiate the wind;

  6. (f) The relative complexity of WR wind initiation may be associated with the extensive turbulent structure inferred from observed variabililty in WR wind emission lines;

  7. (g) Overall, the understanding of WR winds is perhaps best viewed as an “opacity problem”, i.e., identifying the enhanced opacity that can adequately block the radiation flux throughout the wind, and thus drive a WR mass loss that is much greater than from OB stars of comparable luminosity.

Type
Part 2. Models for single star evolution of massive stars: wind + atmosphere + interior
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 157 - 167
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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