a^3}\bigg\}^{\frac{1}{2}} 
\times \bigg\{1-\frac{M_s}{M_{puls} + M_{s}}\bigg\}^{-\frac{1}{2}}$$

where P$_{orb}$ is the orbital period, $a$ is the semi-major axis of the eclipsing system’s orbit and M$_{s}$) is the mass of the secondary star and G is the Newton’s gravitational constant. This expression indicates that the pulsational period of a pulsator in an eclipsing binary is depended up on the orbital period.

We also plot the pulsation periods against the gravities of the pulsating stars in Fig.8, where the pulsational periods are in days and the gravities in CGS units. The open square in this figure shows V404Lyr for which no radial velocities exist, the gravity is estimated from the preliminary mass and radius determined only from the light curves. Therefore it was not used in the calculation of the correlation between the pulsational period and gravity. Gravities were calculated for only six $\gamma$-Dor type pulsators in the close binaries for which radial velocities and photometric light curves exist. A preliminary least squares analysis yields a relationship between the pulsational period and gravity as,

$$log P_{puls} = -0.828(\pm 0.076) \times \log g + 3.385(\pm 0.218)$$

with a correlation coefficient of 0.81. The pulsational periods are decreasing while the surface gravities are increasing, similar to 