Volume 366, Number 2, February I 2001
|Page(s)||585 - 597|
|Section||Interstellar and circumstellar matter|
|Published online||15 February 2001|
The spectral variability of HD 192639 and its implications for the star's wind structure*
Institut d'Astrophysique et de Géophysique, Université de Liège, 5 avenue de Cointe, 4000 Liège, Belgium
2 Ritter Astrophysical Research Center, Toledo, OH 43606, USA
Accepted: 9 November 2000
We report the analysis of an extensive set of spectroscopic data of the O(f) supergiant HD 192639. A Fourier analysis of our time-series reveals a recurrent variability with a "period"of roughly 4.8 days which is most prominent in the absorption components of the He ii λ 4686 and Hα P-Cygni profiles. The same periodicity is also detected in the blue wing of several absorption lines (e.g. Hβ). The variations of the absorption components correspond most probably to a cyclical modulation of the amount of stellar wind material along the line of sight towards the star. The 4.8-day period affects also the morphology of the double-peaked He ii λ 4686 and Hα emission components, although these emission components display also variations on other (mainly longer) time scales. The most likely explanation for the 4.8-day modulation is that this cycle reflects the stellar rotational period (or half this period). We find that the most important observational properties can be explained -at least qualitatively -by a corotating interaction region or a tilted confined corotating wind.
Key words: line: profiles / stars: early-type / stars: mass loss / stars: individual: HD 192639 / stars: variables: general
© ESO, 2001
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