Abstract
As first pointed out by Moskalik and Dziembowski (1992) all β Cephei stars lie within the domain of H–R diagram where к–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.
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Cugier, H. Dziembowski, W.A. and Pamyatnykh, A.A.: 1993, this issue
Dziembowski, W.A. and Pamyatnykh, A.A.: 1993, MNRAS 262, 204
Jerzykiewicz, M., Sterken, C. and Kubiak, M.: 1988, A&AS 72, 449
Moskalik, P. and Dziembowski, W.A.: 1991, A&A 256, L5
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© 1994 Springer Science+Business Media Dordrecht
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Cugier, H., Pigulski, A., Polubek, G., Monier, R. (1994). Multiwavelength Studies of β Cephei Stars. In: Balona, L.A., Henrichs, H.F., Le Contel, J.M. (eds) Pulsation, Rotation and Mass Loss in Early-Type Stars. International Astronomical Union / Union Astronomique Internationale, vol 162. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1030-3_3
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DOI: https://doi.org/10.1007/978-94-011-1030-3_3
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