Hostname: page-component-7479d7b7d-fwgfc Total loading time: 0 Render date: 2024-07-08T06:39:42.387Z Has data issue: false hasContentIssue false
  • English
  • Français

On the Nature of the 41-Day Cycle of RR Lyrae

Published online by Cambridge University Press:  12 April 2016

L. Detre  and
B. Szeidl
L. Detre
Affiliation:
Konkoly Observatory, Budapest, Hungary
B. Szeidl
Affiliation:
Konkoly Observatory, Budapest, Hungary

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.

Photoelectric observations obtained with the 24-in. telescope of the Konkoly Observatory from 1950 to 1972 show that the amplitudes of the changes of the 0.d57 light-curve in the course of the 41-day cycle undergo considerable cyclic variations. The length of the cycles varies between 3.8 and 4.8 yr. A new cycle always begins with a large phase-shift in the 41-day period; afterwards there is generally no further shift during one 4-yr cycle. Following Julia Balázs’ hypothesis, a tentative model is suggested: The 41-day cycle is the rotation period of the star. Magnetic fields concentrated in a limited longitude zone influence the 0.d57 pulsation in such a way that variations in light amplitude and phase arise as aspect effects of the 41-day rotation period. In this way, the 4-yr cycle can be interpreted as the magnetic cycle of the star. The location of the magnetic fields strongly differs in longitude from cycle to cycle causing the observed large phase shifts at the beginning of a new 4-yr cycle.

Type
Part I / General Problems of Variables in Population II Systems
Information
International Astronomical Union Colloquium , Volume 21: Variable Stars in Globular Clusters and in Related Systems , August 1973 , pp. 31 - 34
Copyright
Copyright © Reidel 1973

References

Referensces

Babcock, H. W.: 1955, Publ. Astron. Soc. Pacific 67, 70.Google Scholar
Babcock, H. W.: 1958, Astrophys. J. Suppl, 3, 141.CrossRefGoogle Scholar
Balázs, J.: 1959, Kleine Veröff. Remeis-Sternw. No.27, p26.Google Scholar
Balázs-Detre, J. and Detre, L.: 1962, Kleine Veröff. Remeis-Sternw. No. 34.Google Scholar
Broglia, P. and Masani, A.: 1957, Contr. Oss. Astr. Milano-Merate, Nuova Serie, No.105.Google Scholar
Cocito, G. and Masani, A.: 1960, Contr. Oss. Astr. Torino, Nuova Serie, No. 27.Google Scholar
Detre, L.: 1943, Mitt. Sternw. Ungar. Akad. Wiss. No.17.Google Scholar
Detre, L.: 1961, IAU Trans. XIB, 295.Google Scholar
Detre, L.: 1969, Non-Periodic Phenomena in Variable Stars, Academic Press, Budapest.CrossRefGoogle Scholar
Detre, L.: 1970, Ann. Univ.-Sternw. Wien 29, No. 2, 79.Google Scholar
Hardie, R. H.: 1955, Astrophys. J. 122, 256.CrossRefGoogle Scholar
Onderlicka, B. and Vetsnik, M.: 1968, Astron. Inst. Univ. Brno (Czechoslovakia), Publ. No.8.Google Scholar
Preston, G. W.: 1964, Ann. Rev. Astron. Astrophys. 2,46.CrossRefGoogle Scholar
Preston, G. W., Smak, J., and Paczyński, B.: 1965, Astrophys. J. Suppl. 12, 99.CrossRefGoogle Scholar
Preston, G. W.: 1967, in Cameron, R. C. (ed.), The Magnetic and Related Stars, Mono Book Corp., Baltimore, p. 26.Google Scholar
Szeidl, B.: 1965 Mitt. Sternw. Ungar. Akad. Wiss. No. 58, p74.Google Scholar
Wachmann, A. A.: 1968, Astr. Abh. Hamburg Sternw. Bergedorf 8, No. 114.Google Scholar
Walraven, Th.: 1949, Bull. Astron. Inst. Neth. 11, 17.Google Scholar