The Anticorrelated Nature of the Primary and Secondary Eclipse Timing Variations for Thekeplercontact Binaries

We report a study of the eclipse timing variations in contact binary systems, using long-cadence lightcurves from the Kepler archive. As a first step, observed minus calculated ( O − C ) curves were produced for both the primary and secondary eclipses of some 2000 Kepler binaries. We find ∼390 short-period binaries with O − C curves that exhibit (1) random walk-like variations or quasi-periodicities, with typical amplitudes of ±200–300 s, and (2) anticorrelations between the primary and secondary eclipse timing variations. We present a detailed analysis and results for 32 of these binaries with orbital periods in the range of 0.35 ± 0.05 days. The anticorrelations observed in their O − C curves cannot be explained by a model involving mass transfer, which, among other things, requires implausibly high rates of ∼0.01 M ☉ yr −1 . We show that the anticorrelated behavior, the amplitude of the O − C delays, and the overall random walk-like behavior can be explained by the presence of a starspot that is continuously visible around the orbit and slowly changes its longitude on timescales of weeks to months. The quasi-periods of ∼50–200 days observed in the O − C curves suggest values for k , the coefficient of the latitude dependence of the stellar differential rotation, of ∼0.003−0.013.