Authors:
Chapellier E., Sadsaoud H., Valtier J.C., Garrido R., Sareyan J.P., Le Contel J.M., Alvarez M.
Journal:
Astronomy and Astrophysics
Abstract:
A new investigation of the behaviour of the star 53 Per was performed. New photometric observations allow to confirm two dominant periods p1=2.16d, p2=1.67 d. A third one p3=3.64 d is detected. These long period variations are present in our radial velocities data and in old equivalent width data. The amplitude of the p1 = 2.16d period increases from 1977 to 1991, while the amplitude of the 1.67 d period remains constant. Considering the observational characteristics of the star since 1997, 53 Per clearly belongs to the Slowly Pulsating B stars group as defined by Waelkens (1991) and North & Paltani (1994).
Keywords:
53 Persei; General stars; Individual; Oscillations stars; Stars; Variables