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In this paper, four sets of evolutionary models are computed with differentvalues of the mixing length parameter $\alpha_{\rm p}$ and the overshootingparameter $\delta_{\rm ov}$. The properties of the convective cores and theconvective envelopes are studied in the massive stars. We get threeconclusions: First, the larger $\alpha_{\rm p}$ leads to enhancing theconvective mixing, removing the chemical gradient, and increasing theconvective heat transfer efficiency. Second, core potential $\phi_{\rm c} =M_{\rm c} / R_{\rm c}$ describes sufficiently the evolution of a star, whetherit is a red or blue supergiant at central helium ignition. Third, thediscontinuity of hydrogen profile above the hydrogen burning shell seriouslyaffect the occurrence of blue loops in the Hertzsprung--Russell diagram.

Convection and convective overshooting in stars more massive than 10 $M_\odot$