The Sch\"{o}nberg-Chandrasekhar limit in post main sequence evolution for stars of masses the range $1.4\lesssim M/M_{\odot}\lesssim 6$ gives maximum pressure that stellar core can withstand, once central hydrogen is exhausted. It usually expressed as a quadratic function $1/\alpha$, with $\alpha$ being ratio mean molecular weight to envelope. Here, we revisit this scenarios where balance equat...