Indirect evidence for short period magnetic cycles in W UMa stars

Abstract

Complex period variations of five W UMa type binaries (AB And, OO Aql, DK Cyg, V566 Oph, U Peg) were investigated by analyzing their O--C diagrams, and several common features were found. Four of the five systems show secular period variations at a constant rate on the order of |dP / dt 1/P | ~ 10E-7 1/yr. 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, although the mathematical, and consequently the physical, parameters of these fits are very problematic, as the obtained periods are very close to the length of the total data range. The most interesting feature of the studied O--C diagrams is a low amplitude (2-4 x 10E-3 d) modulation with a period around 18--20 yr in four of the five cases. This phenomenon might be indirect evidence of some magnetic cycle in late-type overcontact binaries as an analog to the observed activity cycles in RS CVn systems.

Accepted for A&A; 11 pages, 9 figures

References in corpus (3)

• Radial Velocity Studies of Close Binary Stars. IX
• The structure of contact binaries
• An Ultraviolet Study of the Short-Period Binary OO Aquilae

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