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The Stability of Cepheid Lightcurves

Published online by Cambridge University Press:  15 February 2018

J.D. Fernie
J.D. Fernie*
Affiliation:
David Dunlap Observatory, Richmond Hill, Ontario, Canada

Abstract

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Published lightcurves of 25 to 40 day classical Cepheids and of BL Herculis stars have been examined closely for evidence of alternating deep and shallow minima, as predicted by Moskalik and Buchler (1991) and Buchler and Moskalik (1992). No such effect has been detected. Two stars, SZ Mon and EN Tra, which are sometimes taken to be classical Cepheids, do show this RV Tauri-like effect, but neither star is, in fact, likely to be a classical Cepheid.

Type
Windows on the Instability Strip
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 422
Copyright
Copyright © Cambridge University Press 1993

References

Buchler, J.R., and Moskalik, P. 1992, ApJ, 391, 736.CrossRefGoogle Scholar
Coulson, I.M., and Caldwell, J.A.R. 1985, So. Afr. Ast. Obs. Circ. No. 9, 1.Google Scholar
Lloyd Evans, T. 1971, The Observatory, 91, 159.Google Scholar
McAlary, C.W., and Welch, D.L. 1986, AJ, 91, 1209.CrossRefGoogle Scholar
Moffett, T.J., and Barnes, T.G. III 1984, ApJS, 55, 389.Google Scholar
Moskalik, P., and Buchler, J.R. 1991, ApJ, 366, 300.CrossRefGoogle Scholar
Pel, J.W. 1976, A&AS, 24, 413.Google Scholar
Stobie, R.S. 1970, MNRAS, 148, 1.Google Scholar