Radiative homology with CNO burning and electron scattering
= Radiative homology with CNO burning and electron scattering
Using the idealized <CNO cycle> law $\epsilon\propto\rho T^{16}$ and constant <electron-scattering opacity>, <homology relations for radiative stars> give
$$
R\propto M^{15/19},\qquad L\propto M^3,\qquad T_{\rm eff}\propto L^{9/76}.
$$
These retain ideal-gas pressure support; significant <radiation pressure> or convection changes the model.