Reference : The spectral variability of HD 192639 and its implications for the star's wind structure
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/15961
The spectral variability of HD 192639 and its implications for the star's wind structure
English
Rauw, Grégor mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) - Sciences spatiales >]
Morrison, N. D. [Ritter Astrophysical Research Center, Toledo, OH 43606, USA]
Vreux, Jean-Marie [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > > ]
Gosset, Eric mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Mulliss, C. L. [Ritter Astrophysical Research Center, Toledo, OH 43606, USA]
1-Feb-2001
Astronomy and Astrophysics
EDP Sciences
366
585-597
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] LINE: PROFILES ; STARS: EARLY-TYPE ; STARS: MASS LOSS ; STARS: INDIVIDUAL: HD 192639 ; STARS: VARIABLES: GENERAL
[en] 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}\ lambda 4686 and Halpha P-Cygni profiles. The same periodicity is also detected in the blue wing of several absorption lines (e.g. Hbeta ). 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}\ lambda 4686 and Halpha 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. Based on observations collected at the Observatoire de Haute Provence, France and the Ritter Observatory, Toledo, USA.
http://hdl.handle.net/2268/15961
10.1051/0004-6361:20000106
http://adsabs.harvard.edu/abs/2001A%26A...366..585R

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