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 |
The Effects of Clumping on UV Wind Line Diagnostics
Derck Massa
STScI/SGT, Inc
Raman Prinja
Dept. of Physics and Astronomy, UCL
By comparing mass loss rates determined from radio, H alpha, and UV resonance lines, it has become reasonably certain that clumping in OB star winds affects empirical determinations of their mass loss rates. We examine three additional UV spectral diagnostics that are sensitive to clumping and, ultimately, may help constrain its nature. They are: 1) doublet ratios of resonance lines; 2) deep cusps near terminal velocity in stars with weak winds; and 3) the ratio of the resonance and radiatively excited state lines of Si IV in certain O9-B0 supergiants. We present examples of each diagnostic and explain why they respond to clumping.
