Spectroscopic Variability of Supergiant Star HD14134, B3Ia

Profile variations in the H α and H β lines in the spectra of the star HD14134 are investigated using observations carried out in 2013–2014 and 2016 with the 2-m telescope at the Shamakhy Astrophysical Observatory. The absorption and emission components of the H α line are found to disappear on some observational days, and two of the spectrograms exhibit inverse P-Cyg profile of H α . It was revealed that when the H α line disappeared or an inversion of the P-Cyg-type profile is observed in the spectra, the H β line is displaced to the longer wavelengths, but no synchronous variabilities were observed in other spectral lines (CII λ 6578.05 Å, λ 6582.88 Å and HeI λ 5875.72 Å) formed in deeper layers of the stellar atmosphere. In addition, the profiles of the H α and H β lines have been analysed, as well as their relations with possible expansion, contraction and mixed conditions of the atmosphere of HD14134. We suggest that the observational evidence for the non-stationary atmosphere of HD14134 can be associated in part with the non-spherical stellar wind.