53-PERSEI - A SLOWLY PULSATING B-STAR

A new investigation of the behaviour of the star 53 Per was performed. New photometric observations allow to confirm two dominant periods p( 1)=2.16 d, p(2)=1.67 d. A third one p(3)=3.64 d is detected. These lon g period variations are present in our radial velocities data and in o ld equivalent width data. The amplitude of the p(1)=2.16d period incre ases from 1977 to 1991, while the amplitude of the 1.67 d period remai ns constant. Considering the observational characteristics of the star since 1997, 53 Per clearly belongs to the Slowly Pulsating B stars gr oup as defined by Waelkens (1991)and North & Paltani (1994).