Spectroscopic study of the Be star phi persei

Abstract

Based on a series of Coude spectra taken with the 188-cm reflector of the Okayama Astrophysical Observatory over an interval of 18 yr, the spectroscopic behavior in the Balmer and HeⅠ λ3888 lines of the binary Be star Ø per (orbital period of 126.696 d) is presented. We have confirmed the following phenomena: (1) the V/R ratio (intensity ratio of violet to red peaks of the double-peaked emission lines) varies synchronously with the binary phase, and its amplitude is about 2; (2) the shell absorption lines become very strong at a phase of around 0.1; (3) there is a remarkable hump in the radial velocity curve of the shell lines near to phase of 0.4 to 0.6; and (4) the peak separations of the emission lines do not vary with the phase, but remain constant.