A LONG-TERM SPECTROSCOPIC STUDY OF THE BE/X-RAY BINARY X-PER (4U-0352+30)

New spectroscopic observations of X Per, the optical counterpart of the steady, pulsating X-ray source 4U 0352 + 30, are presented, covering an interval of more than 2 years. The proposed orbital period of almost-equal-to 580 d, suggested by the regularity of the X-ray outbursts from this system, is not confirmed, although the observations show that the star is probably a velocity variable. The observations have been subjected to a period search procedure, showing that no other periods between 10-600 d are indicated. It is concluded that the amplitude of the orbital motion is too low to have been detected in this study. Results of line variation measurements are presented which show no obvious correlation with the fact that X Per underwent a transition from a Be- to a B-type spectrum during the course of this study.