  The presence of r mode oscillations (global modes of Rossby waves coupled
with buoyancy) in an eclipsing binary is recognized as frequency groups in a
frequency-amplitude diagram obtained from a Fourier analysis of Kepler light
curve data. The frequency at the upper bound of an r-mode frequency group is
close to the rotation frequency of the star. Analysing about eight hundred
Kepler light curves of eclipsing binaries finds about seven hundred cases
showing the signature of r modes. Sometimes two sets of the frequency groups
are found, which indicates the two component stars to have slightly different
rotation frequencies. Plotting thus obtained rotation frequencies with respect
to orbital frequencies, we find that rotation is roughly synchronous to the
orbital frequency if the latter is larger than about 1 c/d, while some stars
rotate super-synchronously in systems with longer orbital periods.
