Computer Science
Scientific paper
Apr 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008cihw.conf...47d&link_type=abstract
Clumping in hot-star winds : proceedings of an international workshop held in Potsdam, Germany, 18. - 22. June 2007. Hamann, Wol
Computer Science
4
Scientific paper
We present the latest results on the observational dependence of the mass-loss rate in stellar winds of O and early-B stars on the metal content of their atmospheres, and compare these with predictions. Absolute empirical rates for the mass loss of stars brighter than 10^{5.2} L_{&sun;}, based on Hα and ultraviolet (UV) wind lines, are found to be about a factor of two higher than predictions. If this difference is attributed to inhomogeneities in the wind this would imply that luminous O and early-B stars have clumping factors in their Hα and UV line forming regime of about a factor of 3-5. The investigated stars cover a metallicity range Z from 0.2 to 1 Z_{&sun;}. We find a hint towards smaller clumping factors for lower Z. The derived clumping factors, however, presuppose that clumping does not impact the predictions of the mass-loss rate. We discuss this assumption and explain how we intend to investigate its validity in more detail.
de Koter Alex
Muijres L.
Vink Jorick S.
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