Structure and Evolution of the Stars

absorption coefficient abundance Ap.J approximation apsidal motion atomic average binaries carbon cycle composition computations consider contraction convective core convective envelopes core solution degeneracy degenerate density derived determined effective temperature electron scattering envelope solution evolutionary phases evolutionary tracks factor fitting conditions function given globular clusters gravitational energy heavier elements helium core Hence Hertzsprung-Russell diagram homogeneous hydrogen burning hydrogen content hydrostatic equilibrium inhomogeneous initial layers luminosity main sequence main-sequence stars mass-luminosity relation massive stars million degrees non-degenerate nuclear energy nuclear processes nuclear transmutations numerical integrations observed obtain occur opacity parameter pressure proton proton-proton reaction quantities radiation flux radiative equilibrium radius red giants represent sequence stars shell solar masses stellar evolution stellar interior stellar models subdwarfs Table temperature gradient thermal equilibrium tion transformation transmutation triple-alpha process upper main sequence upper main-sequence UV plane variables velocity white dwarfs zero zone