been made and precise radial velocities and, therefore, the orbital elements were determined. The number of $\gamma$-Dor type pulsators in the close binaries will be rapidly increased in a few years after the analyses of the huge precise data obtained by space missions such as $CoRot$, $Kepler$, etc.

A decade ago [@soy] suggested a linear relationship between the orbital and pulsation periods for the 20 $\delta$-Sct type pulsators in the classic Algol type systems. This relationship based on observations is confirmed and refined by [@lia] using the data almost quadruple than that of [@soy]. The correlation between the pulsation ($P_{puls}$) and orbital ($P_{orb}$) periods has been theoretically established by [@zhang]. In Table6 we present mass and radius (in solar units), mean density and surface gravity (in CGS units) and pulsation constant (in days) for the pulsating stars in the eclipsing binaries, for which precise photometric and spectroscopic observations are available. The dominant pulsation periods are taken into account and the pulsation constants were calculated using these periods and mean densities. The pulsation constants vary between 0.17 and 0.72, systematically larger than the value of 0.033 days for the radial fundamental modes [@bre; @sta].

In Fig.7 we plot the dominate pulsation 