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Non-Cepheids in the Instability Strip

Published online by Cambridge University Press:  12 April 2016

William P. Bidelman
William P. Bidelman*
Affiliation:
Warner and Swasey Observatory, Case Western Reserve Univ., Cleveland, Ohio 44106

Abstract

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The question of whether non-Cepheids populate the cepheid instability strip has been the subject of much recent interest. Several investigators (see especially Fernie and Hube 1971 and Fernie 1976) have concluded that indeed there are an appreciable number of objects not presently recognized as Cepheids within the strip, though both the size and position of the strip and the placement of supergiants in the H-R diagram are subject to considerable uncertainty. In view of the interest in this matter, I have attempted to shed some light on this situation by simply considering the nature of the stars spectroscopically classified as of high luminosity in spectral classes F and G. For this one needs, of course, a complete sample of the relevant stars, which fortunately is now to some extent available.

Type
Part I. Fundamental Parameters
Information
International Astronomical Union Colloquium , Volume 82: Cepheids: Theory and Observations , 1985 , pp. 83
Copyright
Copyright © Cambridge University Press 1985

References

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Houk, N. and Cowley, A. P. 1975, U. of Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars, Vol. 1 (Ann Arbor: U. of Michigan Dep’t of Astronomy).Google Scholar
Houk, N., Hartoog, M. R., and Cowley, A. P. 1976, Astron. J. 81, 116.10.1086/111862CrossRefGoogle Scholar