Spectral variability of luminous early type stars
I. Peculiar supergiant HD199478
N. Markova and
Received 15 June 2000 / Accepted 8 September 2000
We have obtained time-series of high-quality spectra with high resolution in wavelength (R = of 15000 to 22000) and time ( =1d) of the late-type B supergiant HD199478. The spectra were analysed in terms of line-profile variability (lpv) using contemporary techniques of time-series analysis, such as Temporal Variance Spectrum and the 2d- Discrete Fourier Transform. The profile is found to consist of a highly variable emission core (between -280 and +150 km s-1) superimposed on almost constant, extended (1000 km s-1) emission wings. Due to the lack of strong line-emission, the latter is attributed to electron-scattering in deep atmospheric layers.
The variability manifests itself by variations in velocity and intensity of blue- and red-shifted emission peaks, which result in drastic alterations in the shape of the profile from almost symmetric and unshifted emission, with respect to the stellar rest frame, through blue- or red-shifted asymmetric emission, to double-peaked emission or a reverse P Cygni-type profile. Significant variations in total emissivity (i.e. EW) of the line are also noted, but these variations do not appear to be obviously linked to changes in the line-profile shape. The pattern of variability resembles that in Be-stars - though on a much shorter time scale - and suggests interpretation in terms of an axially symmetric and perturbed stellar wind. Since the time-scale of the V/R variations is found to be 3 to 5 times longer than the radial fundamental pulsation period but consistent with rotational period, rotational modulation as a possible cause for this variability is considered.
Besides variations in , continuous changes in velocity (typical dispersion of 5 km s-1) and strength, i.e. EW, (up to 13% of the mean) of a sample of three absorption lines (, 6578 and ) were also observed. The phenomenon observed is more likely connected to changes in velocity and temperature structures of the stellar photosphere. Pulsation instability as a possible cause of photospheric variability is suggested.
Key words: line: profiles stars: early-type stars: emission-line, Be stars: individual: HD 199478
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© European Southern Observatory (ESO) 2000
Online publication: December 5, 2000