Abstract
We present photometric light curve modelling of four Kepler eclipsing binaries KIC 2720354, KIC 10063044, KIC 11724091 and KIC 8565912. The modelling results show that KIC 10063044 is a semi-detached eclipsing binary, while the other systems are detached eclipsing binaries. Estimated physical parameters of these systems and residuals from the best-fitting light curve models strongly indicate γ Dor type pulsations on the primary components of the target systems. Evaluating the relations between pulsation period (Ppuls) and orbital period (Porb), the force exerted to per gram on the surface of the pulsating star (F/Mpuls) and the fractional radius of the pulsating star (r), we find that linear relations on a logarithmic scale still exist, but with a smaller slope than reported in previous studies.
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