Effective temperature T_eff of the disk, calculated according to Eq. (16). The plot shows five different models, all of which have the same stellar mass of 1.0   M_⊙, but different stellar rotation rates ω = Ω_∗/Ω_K(R_∗). The plot depicts two regions separated by a light grey bar that differ in the radial scaling and enable us to show both the narrow but very distinct peak of the effective temperature in the BL and the nearly constant behaviour in the disk all in one graph.