= Eddington-model convective-core mass fraction
{c}
{title2=$M_c/M=1/(4\nabla_{\rm ad})=\Gamma_2/[4(\Gamma_2-1)]$}
The global Eddington closure $L=(1-\beta)4\pi cGM/\kappa$, combined with a representative <stellar gas-pressure fraction>, makes the exterior <stellar radiative temperature gradient> approximately $M/(4m)$ when the <luminosity> is constant outside the core. Matching it to the <adiabatic temperature gradient> estimates the displayed boundary mass. This is a closure estimate: imposing exactly uniform $\beta$ throughout a finite-mass radiative envelope also conflicts with constant <luminosity>, as described by the <constant-beta radiative-envelope obstruction>.
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