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Nonlinear pulsational behaviour of BW Vulpeculae

Published online by Cambridge University Press:  26 May 2016

P. Moskalik  and
J.R. Buchler
P. Moskalik
Affiliation:
N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
J.R. Buchler
Affiliation:
Department of Physics, University of Florida, Ganesville, FL32611, USA

Extract

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BW Vulpeculae is a large amplitude β Cephei-type star, pulsating with a single period of 0.20104 day. Its nonlinear modeling was first attempted by Pesnell & Cox (1980). Because the true instability mechanism was not known then, the pulsation amplitude was imposed in that study in an arbitrary fashion.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 19 - 20
Copyright
Copyright © Kluwer 1994 

References

Barry, D.C., Holberg, J.B., Forrester, W.T., Polidan, R.S. and Furenlid, I.: 1984, ApJ. 281, 766.Google Scholar
Dziembowski, W.A. and Pamyatnykh, A.A.: 1993, MNRAS 262, 204 Google Scholar
Furenlid, I., Young, A., Meylan, T., Haag, C. and Crinklaw, G.: 1987, ApJ. 319, 264 Google Scholar
Heynderickx, D.: 1991, Ph. D. Thesis, Katholieke Universiteit Leuven.Google Scholar
Iglesias, C.A., Rogers, F.J. and Wilson, B.G.: 1992, ApJ. 397, 717 CrossRefGoogle Scholar
Pesnell, W.D. and Cox, A.N.: 1980, Space Sci. Rev. 27, 337 Google Scholar
Stellingwerf, R.F.: 1974, ApJ. 192, 139 Google Scholar