Physics
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...421..310m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 421, no. 1, p. 310-313
Physics
93
Stellar Mass, Stellar Mass Ejection, Stellar Spectra, Stellar Winds, Wolf-Rayet Stars, Astronomical Models, Astronomical Spectroscopy, Plasma Turbulence, Stellar Physics
Scientific paper
We construct a simple model for the continuum free-free or subordinate line emission from Wolf-Rayet star winds, in which full-scale, compressible, supersonic turbulence is assumed to prevail. Based on observed properties of the turbulent eddies with extrapolation by analogy with Giant Molecular Clouds, such clumpy winds could lead to a decrease in the estimate of the mass-loss rate by a factor approximately greater than 3 compared to homogeneous winds of the same free-free or subordinate line flux. Clumping may be important in all hot stars with winds. In the particular case of the key eclipsing WR + O binary V444 Cygni, the observed difference between the higher values of dot-M traditionally found from the radio free-free emission or the recombination flux of He I 1.08 micrometers assuming homogeneity, and the lower dot-M values from dynamical arguments or polarimetry is found to be a factor approximately greater than 3, in agreement with the above turbulence-based factor. The former methods depend on the square of the density and hence are sensitive to clumping effects, while the latter methods are impervious to density fluctuations and are considered more reliable.
Moffat Anthony F. J.
Robert Carmelle
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