Peculiarities of Line Variability in the Spectrum of κCas. I.Photospheric and Wind Lines HeI

Temporal variations of radial velocities and profiles of the photospheric SiIII, OI I, HeI, H10-Hδ and wind HeIλ5875, 6678 lines were investigated in the spectra κCas. Rapid variabilities (P < 1 day) of radial velocities and line profiles were not detected. Radial velocity variability of all studied lines is mainly caused by non-radial pulsations. In case of photospheric lines the quasi-periodic variations were found for radial velocity variability. For wind lines HeIλ5875, 6678, patterns of temporal variability of radial velocity differ from each other and photospheric lines. Gamma-velocities and amplitudes of radial velocity variability were defined for them.The amplitude of spectrophotometric parameters and radial velocity variations, as well as rate of expansion increases from lower to upper layers of the atmosphere. Emission components are superimposed on line profiles correspondingly at positions of about"135±10.0, "20±20 and 135±10. 0kms"1. They are more obviously seen in the windlines, but their traces are visible in all photoshperic lines. Such a pattern and character of the variability of all the line profiles in the spectrum of κCas how that it is a supergiant which shows the Be phenomenon.