= Stellar radiative temperature gradient
{title2=$\nabla_{\rm rad}=3\kappa L_rP/(16\pi a_{\rm r}cGmT^4)$}
The <radiative temperature gradient> needed to carry a spherical stellar <luminosity> follows by dividing <radiative diffusion in a star> by the <hydrostatic pressure support equation>. It is a logarithmic <pressure> gradient, not $dT/dr$ itself. Comparing it with the <adiabatic temperature gradient> by the <Schwarzschild criterion> determines whether purely radiative transport is locally unstable at uniform composition.
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