Eddington factor and opacity as a function of the temperature inside an initially rotating single 30 M_⊙ star S2 and a primary star in B3 with the same effective temperature log T_eff = 5.11 at almost the end of the evolution. The Eddington factor is defined as , where M(r) is the Lagrangian mass coordinate, κ(r) is the Rosseland mean opacity, and L(r) is the local luminosity (Langer 1997).