Hostname: page-component-8448b6f56d-c4f8m Total loading time: 0 Render date: 2024-04-25T06:16:06.525Z Has data issue: false hasContentIssue false
  • English
  • Français

Pulsations of the Mira-type component in the Symbiotic Binary R Aqr

Published online by Cambridge University Press:  25 May 2016

L. L. Chinarova ,
I. L. Andronov  and
E. Schweitzer
L. L. Chinarova
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

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.

Time series analysis of the brightness variations of R Aqr is based on 1521 visual observations from the AFOEV database. The statistically significant number of harmonics for the mean phase curve is m = 5. The cycle-to-cycle variations of the phase curve are present. The most stable in phase is the maximum, for which no secular period variations detected, but a secondary cycle of P2 = 3955 ± 50d and amplitude (0.032 ± 0.005)P may be suggested.

Type
V. From AGB to Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 344 - 345
Copyright
Copyright © Kluwer 1997 

References

Andronov, I. L., 1994, Odessa Astron. Publ., 7, 49.Google Scholar
Andronov, I. L., 1996, this volume.Google Scholar
Chinarova, L.L., 1995, Astron. Astrophys. Transact., 9, 103.CrossRefGoogle Scholar
Chinarova, L.L., Andronov, I.L., Schweitzer, E., 1994, Odessa Astron. Publ., 7, 103.Google Scholar
Schweitzer, E., 1993, Bull. AFOEV, 64, 14.Google Scholar