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The detached eclipsing binary stars with convective cores provide a good toolto investigate the convective core overshoot. It has been performed on somebinary stars to restrict the classical overshoot model which simply extends theboundary of fully mixed region. However, the classical overshoot model isphysically unreasonable and inconsistent with the helioseismic investigation.An updated model of the overshoot mixing was established recently. There is akey parameter in the model. In this paper, we use the observations of foureclipsing binary stars, i.e., HY Vir, YZ Cas, $\rm{\chi^2}$ Hya and VV Crv, toinvestigate the suitable value for the parameter. It is found that thesuggested value by the calibrations on eclipsing binary stars is same as therecommended value by other ways. And we have studied the effects of the updatedovershoot model on the stellar structure. The diffusion coefficient of theconvective/overshoot mixing is very high in the convection zone, then quicklydecreases near the convective boundary, and exponentially decreases in theovershoot region. The low value of the diffusion coefficient in the overshootregion leads to weak mixing and the partially mixed overshoot region. Thesemi-convection, which appears in the standard stellar models of low-mass starswith convective core, is removed by the partial overshoot mixing.

Calibrating the updated overshoot mixing model on eclipsing binary stars: HY Vir, YZ Cas, X2 Hya & VV Crv