Wind Inhomogeneities in Wolf-Rayet Stars. II. Investigation of Emission-Line Profile Variations
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Cites methods from "Wind Inhomogeneities in Wolf-Rayet ..."
...Physical models of such lpv interpreted in terms of clumps generated by the line-driven instability have been provided by Dessart and Owocki (2002a,b), where thla ter study extends the Lepine and Moffat (1999) wavelet formalism to modeling lpv from hy- drodynamic simulations....
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...Lepine and Moffat (1999) monitored the line-profile variations in the HeII emission lines of WN stars and in CIII emission lines of WC stars, and studied these variations by means of a detailed wavelet analysis....
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470 citations
Cites background from "Wind Inhomogeneities in Wolf-Rayet ..."
...One reason is the discovery that WR stars are highly clumped (e.g. Moffat & Robert 1994, Lepine & Moffat 1999), which has resulted in a downward revision of the observed WR mass-loss rates (e.g. Hamann & Koesterke 1998)....
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359 citations
Cites background from "Wind Inhomogeneities in Wolf-Rayet ..."
...This may relate to the very strong clumping found observationally in Wolf-Rayet winds (Lépine & Moffat 1999; Marchenko et al. 2006), and may be required for an understanding of the very high mass-loss rates of Wolf-Rayet stars (Eichler et al. 1995; Kato & Iben 1992; Heger & Langer 1996)....
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...So far this is best documented for Wolf-Rayet (WR) stars, where line variability on time scales of minutes to hours is thought to constitute direct evidence of outflows that are clumped already in the acceleration zone near the base of the wind (Lépine & Moffat 1999)....
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References
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...Recently, some attempts have been made to relax certain assumptions of the standard model (Hillier 1996, and references therein), and spectral analysis using clumped wind models has been attempted (Schmutz 1997 ; Hillier & Miller 1998)....
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643 citations
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...This might be explained with shocks propagating toward the star, in the wind rest frame, like the ““ reverse shocks ÏÏ found by Owocki et al. (1988) in one-dimensional simulations of radiatively driven winds....
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Additional excerpts
...On the other hand, the He II j5411 line in the WN stars is likely not to be optically thin, which means that the estimated size and location of the LER will be biased by the fact that optically thick lines tend to be naturally rounded (Castor 1970)....
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