Abstract
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.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
References
Barry, D.C., Holberg, J.B., Forrester, W.T., Polidan, R.S. and Furenlid, I.: 1984, ApJ. 281, 766.
Dziembowski, W.A. and Pamyatnykh, A.A.: 1993, MNRAS 262, 204
Furenlid, I., Young, A., Meylan, T., Haag, C. and Crinklaw, G.: 1987, ApJ. 319, 264
Heynderickx, D.: 1991, Ph. D. Thesis, Katholieke Universiteit Leuven.
Iglesias, C.A., Rogers, F.J. and Wilson, B.G.: 1992, ApJ. 397, 717
Pesnell, W.D. and Cox, A.N.: 1980, Space Sci. Rev. 27, 337
Stellingwerf, R.F.: 1974, ApJ. 192, 139
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 1994 Springer Science+Business Media Dordrecht
About this paper
Cite this paper
Moskalik, P., Buchler, J.R. (1994). Nonlinear Pulsational Behaviour of BW Vulpeculae. 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_4
Download citation
DOI: https://doi.org/10.1007/978-94-011-1030-3_4
Publisher Name: Springer, Dordrecht
Print ISBN: 978-0-7923-3045-5
Online ISBN: 978-94-011-1030-3
eBook Packages: Springer Book Archive