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Cycle-to-cycle changes in the Mira-type star RT Cyg

Published online by Cambridge University Press:  25 May 2016

V. I. Marsakova ,
I. L. Andronov  and
E. Schweitzer
V. I. Marsakova
Affiliation:
1Department of Astronomy, Odessa State University, Ukraine
I. L. Andronov
Affiliation:
1Department of Astronomy, Odessa State University, Ukraine
E. Schweitzer
Affiliation:
2AFOEV, Strasbourg, France

Abstract

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The moments of 82 maxima and 76 minima are used for the correlation analysis of the characteristics of the individual cycles. 5 not trivial correlations were found. The characteristic time of the secular decrease of the period is |P/P| = (23.4 ± 4.3) · 103 yrs, but decade–scale and cycle–to–cycle variations are also present.

Type
V. From AGB to Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 358
Copyright
Copyright © Kluwer 1997 

References

Andronov, I. L., 1994, Odessa Astron. Publ., 7, 49.Google Scholar
Marsakova, V. I., Andronov, I. L., 1996, Odessa Astron. Publ., 9, in press.Google Scholar
Schweitzer, E.: 1993, Bull. AFOEV, 64, 14.Google Scholar