type pulsating variables in the eclipsing variables are: V551Aur, VZCVn, V2094Cyg, V404Lyr, Corot100866999, Corot102918586, Corot102937335, Corot102980178,KIC04544587, KIC11285625.

The $\gamma$ Doradus and $\delta$ Scuti type pulsators share a similar parameter space in the Hertzsprung-Russell (HR) diagram. While the $\delta$ Sct stars are believed to be mostly low-radial-order pressure mode pulsators [@bre00], the $\gamma$ Dor stars are high-radial-order gravity mode pulsators [@kaye]. [@handler02] showed that the $\delta$ Sct and $\gamma$ Dor type pulsating stars are separated by the values of their pulsation constants. While the $\delta$ Sct pulsators have pulsation constant of $Q\sim0.03$ days, the known $\gamma$ Dor pulsators all have $Q$ $>$ 0.23 days.

Therefore, we started to search any periodic light variations in the system. To investigate the intrinsic light variations of the components in eclipsing binary systems, the best-fit binary star model was subtracted from the light curve. This leaves the stellar pulsations, random noise, systematic calibration noise, and any slight mismatches between the model and actual binary star light curve. In these circumstances, frequency analysis was performed on the residuals of the system, in the region 0–3 d$^{-1}$, where the most of the dominant pulsation frequencies are found. In order to generate the frequency spectrum of residual data, 