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2003MNRAS.346..963O - Mon. Not. R. Astron. Soc., 346, 963-967 (2003/December-2)
WR 7a: a V Sagittae or a qWR star ?
OLIVEIRA A.S., STEINER J.E. and CIESLINSKI D.
Abstract (from CDS):
Contrary to what is seen in V Sagittae stars, optical photometric monitoring shows very little, if any, flickering. We found evidence of periodic variability. The most likely photometric period is Pphot0.227(±14) d, while radial velocities suggest a period of Pspec0.204(±13) d. One-day aliases of these periods can not be ruled out. We call attention to similarities with HD 45166 and DI Cru ( WR 46), where multiple periods are present. They may be associated to the binary motion or to non-radial oscillations.
In contrast to a previous conclusion by Pereira et al., we show that WR 7a contains hydrogen. The spectrum of the primary star seems to be detectable as the Nv 4604Åabsorption line is visible. If so, it means that the wind is optically thin in the continuum and that it is likely to be a helium main sequence star.
Given the similarity to HD 45166, we suggests that WR 7a may be a qWR - quasi Wolf-Rayet - star. Its classification is WN4h/CE in the Smith, Shara & Moffat three-dimensional classification system.
Abstract Copyright: 2003 RAS
Journal keyword(s): stars: emission-line, Be - stars: fundamental parameters - stars: individual: WR 7a - stars: Wolf-Rayet
Simbad objects: 7
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