Barbosa |
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Bastian |
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Blum |
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Brott |
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Caballero |
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Chen |
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Chita |
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Chu |
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Churchwell |
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Corcoran |
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Crowther |
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Damineli et al |
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Damineli |
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Fullerton |
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Gagne |
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Gallagher |
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Garcia |
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Garmany |
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Georgiev |
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Hamann |
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Hillier |
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Howarth |
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Indebetouw |
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Kobulnicky |
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Koenigsberger |
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Lang |
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Leitherer |
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Lennon |
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Levesque |
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Linder |
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Maeder |
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Mahy |
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Massa |
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Massey |
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McSwain |
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Moffat |
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Moises |
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Morrell |
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Morris |
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Naze |
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Nieva |
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Olsen |
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Oskinova |
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Owocki |
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Penny |
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Przybilla |
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Skinner |
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Smith |
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Soderberg |
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Teodoro |
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Testor |
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Townsley |
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Vacca |
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Vink |
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Wachter |
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Walborn |
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Wallerstein |
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Whelan |
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Williams |
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Willis |
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Wing |
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Wolff |
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van den Heuvel |
Macroclumping in winds of massive stars
Lidia Oskinova
Universtiy of Potsdam
Wolf-Rainer Hamann
University of Potsdam
Conventionally, stellar wind models account for the inhomogeneity of stellar winds in the approximation of small-scale structures that are optically thin at all wavelength. This convenient approximation is not supported observationally and not predicted theoretically. Specifically, for the cores of strong lines one can expect that the clump optical depth is not necessarily small. This situation is accounted for in the macroclumping approach. For a realistic choice of parameters, we demonstrate how this reduces the wind opacity and affects the emergent spectrum. The reported discrepancy between the resonance-line and recombination-line mass-loss diagnostics can be resolved when macroclumping is accounted for. We demonstrate the effect of macroclumping on spectral lines from O and WR stars in the X-ray, UV, and optical wavelength range.
