Consequences of clumping in hot-star winds

Details Consequences of clumping in hot-star winds Consequences of clumping in hot-star winds

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.221..467m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 221, no. 1-2, p. 467-479

Astronomy and Astrophysics

Astronomy

6

Massive Stars, Stellar Mass, Stellar Physics, Stellar Systems, Stellar Winds, Wolf-Rayet Stars, Anisotropy, Binary Stars, Iue, Mass Distribution, Mass Spectroscopy, Scaling Laws, Spaceborne Astronomy, Turbulence, Ultraviolet Spectra

Scientific paper

It seems more and more likely that one will have to abandon the paradigm of smooth outflows from (hot) stars in favor of a clumpy structure, possibly in a fractal-like hierarchy on all scales. Observationally, this is best established for Wolf-Rayet star winds (e.g. scaling laws, mass-spectrum, anisotropy,...), for which the consequences of clumping are discussed. These include four broad categories, which are outlined in this review: (1) an ideal laboratory for studying time-dependent astrophysical turbulence, (2) potential tracers of hot-wind global structure parameters, (3) reduced mass-loss rates, and (4) impact on massive binary studies.

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