Detection of a 1.59 h period in the B supergiant star HD 202850

• Published in: Astronomy and astrophysics (Berlin) Vol. 542; p. L32
• Main Authors: Kraus, M., Tomić, S., Oksala, M. E., Smole, M.
• Format: Journal Article
• Language: English
• Published: Les Ulis EDP Sciences 01.06.2012
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology; stars: atmospheres; stars: early-type; stars: individual: HD 202850; stars: oscillations; supergiants; stars: atmospheres; stars: individual: HD 202850; B stars; Line shape; Variability; Time series; Stellar pulsations; Massive stars; Early type stars; stars: early-type; stars: oscillations; Short term variation; Supergiant stars; Instability; Stellar rotation; supergiants; Optical spectrum
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/201219319

Context. Photospheric lines of B-type supergiants show variability in their profile shapes. In addition, their widths are much wider than can be accounted for purely by stellar rotation. This excess broadening is often referred to as macroturbulence. Both effects have been linked to stellar oscillations, but B supergiants have not been systematically searched yet for the presence of especially short-term variability caused by stellar pulsations. Aims. We have started an observational campaign to investigate the line profile variability of photospheric lines in a sample of Galactic B supergiants. These observations aim to improve our understanding of the physical effects acting in the atmospheres of evolved massive stars. Methods. We obtained four time-series of high-quality optical spectra for the Galactic B supergiant HD 202850. The spectral coverage of about 500 Å around Hα encompasses the Si ii λλ6347,6371, and the He i λ6678 photospheric lines. The line profiles were analysed by means of the moment method. Results. The time-series of the photospheric Si ii and He i lines display a simultaneous, periodic variability in their profile shapes. Proper analysis revealed a period of 1.59 h in all three lines. This period is found to be stable with time over the observed span of 19 months. This period is much shorter than the rotation period of the star and might be ascribed to stellar oscillations. Since the star seems to fall outside the currently known pulsational instability domains, the nature of the discovered oscillation remains unclear.