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Astron. Astrophys. 331, 1046-1050 (1998)

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53 Persei: a slowly pulsating B star *

E. Chapellier 1, H. Sadsaoud 2, J.C. Valtier 1, R. Garrido 3, J.P. Sareyan 1, J.M. Le Contel 1 and M. Alvarez 4

1 Observatoire de la Côte d'Azur, CNRS UMR 6528, B.P. 4229, F-06304 Nice Cedex 04, France
2 Centre de Recherche en Astronomie Astrophysique et Geophysique, B.P. 63, Bouzareah, 16340 Alger, Algeria
3 Instituto de Astrofisica de Andalucia, Apartado 2144, E-18080 Granada, Spain
4 Observatorio Astronomico National, UNAM, Apdo. 877 Ensenada, B.C., 22800, Mexico

Received 4 August 1997 / Accepted 20 November 1997


A new investigation of the behaviour of the star 53 Per was performed. New photometric observations allow to confirm two dominant periods p1 =2.16 d, 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 = 2.16 d 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).

Key words: stars: variables: general stars: oscillations stars: individual: 53 Persei

* spectroscopic observations performed at the Haute Provence Observatory

Send offprint requests to: E. Chapellier

© European Southern Observatory (ESO) 1998

Online publication: March 3, 1998