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Variable Be Stars in h and χ Persei

Published online by Cambridge University Press:  23 September 2016

C.L. Waelkens ,
P. Lampens ,
J. Cuypers ,
J. Denoyelle ,
D. Heynderickx ,
F. Rufener  and
P. Smeyers
C.L. Waelkens
Affiliation:
Astronomisch Instituut Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3030 Heverlee, (Belgium)
P. Lampens
Affiliation:
Astronomisch Instituut Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3030 Heverlee, (Belgium)
J. Cuypers
Affiliation:
Astronomisch Instituut Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3030 Heverlee, (Belgium)
J. Denoyelle
Affiliation:
Koninklijke Sterrenwacht van België, Ringlaan 3, B-1180 Brussel, (Belgium)
D. Heynderickx
Affiliation:
Astronomisch Instituut Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3030 Heverlee, (Belgium)
F. Rufener
Affiliation:
Observatoire de Genève, 51 Chemin des Maillettes, CH-1290 Sauverny (Switzerland)
P. Smeyers
Affiliation:
Astronomisch Instituut Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3030 Heverlee, (Belgium)

Extract

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The double cluster h and χ Persei has since long been known to be rich in Be stars (Trumpler, 1926). It belongs to an age group in which various types of variable stars occur (Mermilliod, 1981). Other clusters of this age group are NGC 3293, the cluster that is richest in β Cephei variables (Balona and Engelbrecht, 1983), IC 2581, NGC 4755, and NGC 6871. The comparison of the characteristics of variable stars in all these clusters and in clusters of other age groups could reveal to which extent the cluster stellar content is determined by age and by other parameters, such as galactic location, and so metallicity. Since h and χ Persei are very rich clusters that have not yet been studied intensively as far as stellar variability is concerned (Percy, 1972), we have undertaken a study of the photometric variability of the brightest stars in the double cluster. Our first interest was to detect β Cephei variables, but it rapidly turned out that the double cluster contains a considerable amount of highly variable Be stars.

Type
V. Evolutionary Status of Be Stars
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 505 - 508
Copyright
Copyright © Cambridge University Press 1987

References

Balona, L.A., Engelbrecht, C. (1983). Mon. Not. R. Astron. Soc. 202, 293.Google Scholar
Mermilliod, J.-C. (1981). Astron. Astrophys. Suppl. Ser. 44, 467.Google Scholar
Percy, J.R. (1972). Publ. Astron. Soc. Pacific 84, 420.Google Scholar
Trumpler, R.J. (1926). Publ. Astron. Soc. Pacific 38, 350.Google Scholar