Indirect evidence for short period magnetic cycles in overcontact binary stars

Details Indirect evidence for short period magnetic cycles in overcontact binary stars Indirect evidence for short period magnetic cycles in overcontact binary stars

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006padeu..17..109b&link_type=abstract

In: Proceedings of the 4th Workshop of Young Researchers in Astronomy & Astrophysics; Budapest, Hungary, 11-13 January, 2006; Pu

Astronomy and Astrophysics

Astrophysics

Scientific paper

Complex period variations of five W UMa type binaries (AB And, OO Aql, DK Cyg, V566 Oph, U Peg) were investigated by the analysis of their O-C diagrams, and several common features were found. Four of the five systems show secular period variations at a constant rate in the order of |dot{P}_{sec}/P|˜10^{-7} y^{-1}. In the case of AB And, OO Aql and U Peg a high-amplitude, nearly one-century long quasi-sinusoidal pattern was also found. It might be explained as light-time effect, or by some magnetic phenomena. The most interesting feature of the studied O-C diagrams is a low amplitude (˜2-4×10^{-3} d) modulation with a period around 18-20 yr in four of the five cases. This phenomenon might be an indirect evidence of some magnetic cycle in late-type overcontact binaries as an analog to the observed activity cycles in RS CVn systems.

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