Hostname: page-component-7479d7b7d-m9pkr Total loading time: 0 Render date: 2024-07-10T16:32:34.531Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectroscopy of Overluminous Cepheids in the Magellanic Clouds

Published online by Cambridge University Press:  04 August 2017

Horace A. Smith  and
Leo Connolly
Horace A. Smith
Affiliation:
Michigan State University
Leo Connolly
Affiliation:
Southeast Missouri State University

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The Small Magellanic Cloud is known to contain types of short period Cepheid variable stars not yet discovered in either the Large Magellanic Cloud or, with the exception of a single star, in the Galaxy. These variables can be divided into two categories: anomalous Cepheids and Wesselink-Shuttleworth (WS) stars. The former, which have also been found in dwarf spheroidal systems and in the globular cluster NGC 5466, have periods of 0.4–3 days, but average 0.7–1.0 mag. brighter than RR Lyrae and BL Her stars of equal period. The stars we call WS stars have periods less than about 1.1 day and, at MV = −1 to −2, are brighter than anomalous Cepheids of equal period.

Type
Stellar Populations
Information
Symposium - International Astronomical Union , Volume 108: Structure and Evolution of the Magellanic Clouds , 1984 , pp. 223 - 224
Copyright
Copyright © Reidel 1984 

References

Butler, D. 1975. Astrophys. J. 200, pp. 68.Google Scholar
Butler, D., Demarque, P., and Smith, H. A. 1982. Astrophys. J. 257, pp. 592.CrossRefGoogle Scholar
Connolly, L. P. 1980. Sp. Sci. Rev. 27, pp. 443.Google Scholar
Connolly, L. P. 1982. Pulsations in Classical and Cataclysmic Variable Stars, ed. by Cox, J. P. and Hansen, C. J., pp. 188.Google Scholar
Preston, G. W. 1959. Astrophys. J. 130, pp. 507.Google Scholar
Wesselink, A. J. and Shuttleworth, M. 1965. M.N.R.A.S. 130, pp. 433.Google Scholar