 Fixed-radius-core shell-burning luminosity relation

Use a Kramers radiative-zero envelope around a stellar core and specific heating $ϵ={ϵ}_0\rho T^{67/4}$. Since $\rho \propto C{T}^{13/4}$ and $T\propto M_c/r$, $ϵ\propto C{r}^{-20}$ and $ϵ(1.05R_c)/ϵ(R_c)=1.05^{-20}\simeq 0.377$. The volume heating is $\rho ϵ\propto C^2{T}^{93/4}$. Integrating $4\pi r^2\rho ϵ$ from $R_c$ outwards gives $L\propto C^2{M}_c^{93/4}{R}_c^{-81/4}$, while radiative transport gives $C^2\propto M_c/L$. Therefore $L^2\propto M_c^{97/4}{R}_c^{-81/4}$, or $L\propto M_c^{97/8}{R}_c^{-81/8}$. For a core sequence with fixed $R_c$, the mass exponent is $97/8$. The steep integrand confines most heating to a thin shell; using the exterior constant-luminosity profile throughout it estimates the coefficient rather than resolving the shell structure.