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Multiwavelength studies of β Cephei stars

Published online by Cambridge University Press:  26 May 2016

H. Cugier ,
A. Pigulski ,
G. Polubek  and
R. Monier
H. Cugier
Affiliation:
Astronomical Institute, Wrocław University, Kopernika 11, 51-622 Wrocław, Poland
A. Pigulski
Affiliation:
Astronomical Institute, Wrocław University, Kopernika 11, 51-622 Wrocław, Poland
G. Polubek
Affiliation:
Astronomical Institute, Wrocław University, Kopernika 11, 51-622 Wrocław, Poland
R. Monier
Affiliation:
IUE Observatoty VILSPA, P.O. Box-Apartado 50727, Madrid 28080, Spain

Extract

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As first pointed out by Moskalik and Dziembowski (1992) all β Cephei stars lie within the domain of H–R diagram where κ-mechanism effectively drives pulsations in the stellar layers with T ≈ 2×105 K. For most of these objects a chemical composition described by X = 0.70 and Z = 0.02 is sufficient to account for the pulsations, cf. Dziembowski and Pamyatnykh (1993). Recently, Cugier, Dziembowski and Pamyatnykh (1993) have investigated how the present knowledge about nonadiabatic observables of β Cephei stars affects methods of identification of the spherical harmonic degree, l. They found that good photometric and radial velocity data should result in unambiguous identification of l. Cugier, Dziembowski and Pamyatnykh also concluded that nonadiabatic observables can be used to obtain mean stellar parameters of pulsating stars.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 17 - 18
Copyright
Copyright © Kluwer 1994 

References

Cugier, H. Dziembowski, W.A. and Pamyatnykh, A.A.: 1993, this issue Google Scholar
Dziembowski, W.A. and Pamyatnykh, A.A.: 1993, MNRAS 262, 204 Google Scholar
Jerzykiewicz, M., Sterken, C. and Kubiak, M.: 1988, A&AS 72, 449 Google Scholar
Moskalik, P. and Dziembowski, W.A.: 1991, A&A 256, L5 Google Scholar