Nonstationarity of the atmosphere of α Cyg: II. Variability of the ion and H β line profiles

Details Nonstationarity of the atmosphere of α Cyg: II. Variability of the ion and H β line profiles Nonstationarity of the atmosphere of α Cyg: II. Variability of the ion and H β line profiles

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007astbu..62...52r&link_type=abstract

Astrophysical Bulletin, Volume 62, Issue 1, pp.52-61

Astronomy and Astrophysics

Astrophysics

5

97.10.Ex, 97.30.Dg

Scientific paper

We report an efficient method for analyzing the radial-velocity and line-profile variability. We show that a detailed analysis of the variations of line profiles and velocity field in the stellar atmosphere requires the radial velocities to be measured separately for the blue and red halves of the absorption lines at different levels of their residual intensity. We applied this method to 120 CCD spectra taken in 1998 99 with the coude echelle spectrograph attached to the 2-m telescope of Shemakha Astronomical Observatory of National Academy of Sciences of Azerbaijan and analyzed the variations of the radial velocities and profiles of ion and H β lines in the spectrum of α Cyg. In the case of ion lines both halves of the absorption profile exhibit synchronous radial-velocity variations at all levels of line intensity. In the case of the H β line, which forms in the layers where stellar wind originates, the pattern of radial-velocity variations differs for the blue and red halves of the absorption profile. The variability pattern is the same at all levels in the red half of the profile, the blue half of the profile exhibits different variability patterns at different levels of residual line intensity. Identification and analysis of such variations allows us to study the nature of stellar-wind variability in the region of wind formation. The spectrum of α Cyg showed no line-profile or radial-velocity variations for six days in both halves of the absorption contour at all levels of line intensity. The star was in the quiescent phase.

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