SPECTRAL STUDY OF THE HERBIG Ae STAR HD 31648. THE Hα AND Hβ EMISSION LINES

We present the results of observations of the Hα and Hβ lines in spectrum of Herbig Ae star HD 31648. Seven spectra from the Be Stars Spectra Database, with a spectral resolution of R ≈ 11,000, were used, along with three spectra obtained using the 2-m telescope at the Shamakhi Astrophysical Observatory with the Shamakhi Fiber Echelle Spectrograph (R ≈ 28,000). In the spectra at our disposal, the Hα line is predominantly observed as a P Cyg III type profile, characterized by a line intensity ratio of Ib/Ir≪1 and in two cases it was observed as a classical P Cyg type profile – a red-shifted emission peak with blue-shifted absorption. There is no correlation in the changes in the intensity of the blue (Ib) and red (Ir) components. The blue component undergoes the greatest changes, and variability is also present in the intensity of the red emission peak. The Hβ line profile in the central part shows a P Cyg – type structure with wide photospheric wings. The red emission component of the Hβ line shows strong variability, which correlated with the red emission component of the Hα line. In general, variability in the profiles of the Hα and Hβ lines occur synchronously. In the work, a comparative analysis of the behavior of the Hα and Hβ lines is carried out using similar data from published data.