We present spectroscopic and photometric analysis of the eclipsing binary KIC 7385478 .
We find that the system is formed by F1V + K4III-IV components .
Combining results from analysis of spectroscopic data and Kepler photometry , we calculate masses and radii of the primary and the secondary components as M _ { 1 } = 1.71 \pm 0.08 M _ { \odot } , M _ { 2 } = 0.37 \pm 0.04 M _ { \odot } and R _ { 1 } = 1.59 \pm 0.03R _ { \odot } , R _ { 2 } = 1.90 \pm 0.03R _ { \odot } , respectively .
Position of the primary component in HR diagram is in the region of \gamma Doradus type pulsators and residuals from light curve modeling exhibit additional light variation with a dominant period of \sim 0.5 day .
These are clear evidences of the \gamma Doradus type pulsations on the primary component .
We also observe occasional increase in amplitude of the residuals , where the orbital period becomes the most dominant period .
These may be attributed to the cool star activity originating from the secondary component .