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Main-sequence broadening, Be stars, and stellar rotation in h and χ Persei*

Published online by Cambridge University Press:  26 May 2016

J. Denoyelle ,
C. Aerts  and
C. Waelkens
J. Denoyelle
Affiliation:
Royal Observatory, Ringlaan 3, B-1180 Brussels, Belgium
C. Aerts
Affiliation:
Instituut voor Sterrenkunde, Celestijnenlaan 200 B, B-3001 Leuven, Belgium
C. Waelkens
Affiliation:
Instituut voor Sterrenkunde, Celestijnenlaan 200 B, B-3001 Leuven, Belgium

Extract

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The double cluster h and x Persei is one of the richest clusters containing early-B stars, and therefore is important for observational and theoretical studies on the fundamental parameters of massive stars. The colour-magnitude diagram of the double cluster shows an important scatter (see Figure 1). It has long been known that h and x Persei are extremely rich in Be stars (Slettebak 1968). Our previous contention (Waelkens et al. 1990) that the large-amplitude variable stars we discovered are also Be stars, could be confirmed for a few objects. Rotation velocities for stars in h and x Persei are usually high, which is not surprising in view of the large fraction of Be stars.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 151 - 152
Copyright
Copyright © Kluwer 1994 

References

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