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Pulsations and declines of RCB stars

Published online by Cambridge University Press:  15 February 2018

P.L. Cottrell  and
W.A. Lawson
P.L. Cottrell
Affiliation:
Mount John University Observatory, Dept of Physics & Astronomy, University of Canterbury, Christchurch, New Zealand
W.A. Lawson
Affiliation:
Dept of Physics, University College ADFA, UNSW, Canberra, Australia

Abstract

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We have continued to observe many of the R Coronae Borealis (RCB) stars and other related hydrogen-deficient carbon stars. We wish to more fully investigate the photometric and spectroscopic properties of these peculiar stars.

The UBVRI photometric data (acquired at Mount John University Observatory, MJUO) are being used to investigate whether the periods determined by Lawson et al. (1990), based on time intervals of up to 1100 d, are still evident in the larger datasets which now cover time intervals of up to 2200 d.

The long time baseline of photometric observations that we have been able to acquire has enabled us to accumulate an extensive database of decline photometry. These are used to investigate links with the pulsations at maximum light in order to get a better understanding of this remarkable phenomenon.

Type
Beyond the Classical Instability Strip
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 212 - 213
Copyright
Copyright © Cambridge University Press 1993

References

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Lawson, W.A., Cottrell, P.L., Gilmore, A.C., Kilmartin, P.M., 1992, MNRAS 256, 347.Google Scholar
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