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- Title
Spectral and photometric studies of the Wolf-Rayet star WR 134 = HD 191765.
- Authors
Rustamov, D.; Cherepashchuk, A.
- Abstract
The results of spectral and photometric observations of the Wolf-Rayet star WR 134 = HD 191765 performed at the N. Tusi Shamakha Astrophysical Observatory (ShAO) of the National Academy of Sciences of Azerbaijan in 2006-2010 are presented. The spectral observations were carried out at the ShAO Zeiss-2000 telescope with an echelle spectrometer. Thirty-four echelle spectrograms of WR 134 were obtained. Profiles of the five strongest emission lines were analyzed: HeII 4859, HeII 5411, CIV 5808, HeI 5875, and (HeII+H α) 6560. Various parameters of these emission lines are determined: their equivalent widths, radial velocities, central intensities, and half-widths. Only the radial velocity was found to be variable. Variability of the shapes of all emission-line profiles was found, but the largest changes are observed for the (HeII+H α) 6560 emission band. Photometric observations were carried out at the ShAO Zeiss-600 telescope using an Alta U-47 CCD array (1024 × 1024 pixels) in the V filter of the photometric UBV system. Photometric observations were carried out on 18 nights, with from 100 to 300 measurements made during each night. The mean V magnitudes of WR 134 and a control star were determined for each night. Variability of WR 134 was detected, both within a night and during the entire observation period. The exposure time varied from 1 to 6 s on different nights. A statistical analysis of the mean magnitudes indicated that this series contains a peak at a frequency of ν = 0.530 day, corresponding to the period P = 1.887. This period is interpreted as the manifestation binarity for this star. It is suggested that the secondary component of the system may be a low-mass optical K-M star.
- Subjects
ASTRONOMICAL photometry; WOLF-Rayet stars; TELESCOPES; SPECTROGRAMS; UBV system (Astronomy); QUANTITATIVE research; LOW mass stars; RADIAL velocity of stars; K stars; M stars
- Publication
Astronomy Reports, 2012, Vol 56, Issue 10, p761
- ISSN
1063-7729
- Publication type
Article
- DOI
10.1134/S1063772912100058