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1981-82 Observations of the Beat Cepheid U Trianguli Australis

Published online by Cambridge University Press:  25 April 2016

D. J. Faulkner  and
R. R. Shobbrook
D. J. Faulkner
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
R. R. Shobbrook
Affiliation:
Chatterton Department of Astronomy, University of Sydney
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Extract

The nature and cause of the double-mode (DM) pulsation in beat Cepheid variable stars is still a matter of considerable uncertainty. Recently, evidence has been accumulating that the relative energy of the two modes in any particular star may be a slowly varying function of time. For TU Cas, Hodson, Stellingwerf and Cox (1979) have found that the first overtone amplitude has been decreasing over a 67 year timebase, while the present authors (Faulkner and Shobbrook 1979) have reported an increase in overtone energy in U TrA over 20 years. Observational details of the form of the mode energy changes may be helpful in obtaining a better understanding of these stars (see Shobbrook and Faulkner 1982). Our present observations of U TrA have been obtained to investigate its energy changes more fully.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 5 , Issue 2 , 1983 , pp. 217 - 219
Copyright
Copyright © Astronomical Society of Australia 1983

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References

Faulkner, D. J., and Shobbrook, R. R., Astrophys. J., 232, 197 (1979).Google Scholar
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