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High-resolution spectroscopy of Beta Cephei stars

Published online by Cambridge University Press:  26 May 2016

C. Waelkens ,
H. Van Winckel  and
K. de Mey
C. Waelkens
Affiliation:
Instituut voor Sterrenkunde Celestijnenlaan 200B, B-3001 Leuven (Belgium)
H. Van Winckel
Affiliation:
Instituut voor Sterrenkunde Celestijnenlaan 200B, B-3001 Leuven (Belgium)
K. de Mey
Affiliation:
Instituut voor Sterrenkunde Celestijnenlaan 200B, B-3001 Leuven (Belgium)

Abstract

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We give a progress report on an observational program intended to determine detailed chemical abundances of β Cephei stars and constant stars with similar temperature and gravity. There is some evidence that non-variable stars have a lower metal content than variables, as the recently found pulsation mechanism would suggest.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 27 - 28
Copyright
Copyright © Kluwer 1994 

References

The References

Balona, L.A., 1993, Monthly Notices of the RAS256, 425 CrossRefGoogle Scholar
Sterken, C., Jerzykiewicz, M., 1988, Monthly Notices of the RAS235, 565 CrossRefGoogle Scholar