Temperature profile of the outermost layers of a 110 M_⊙ star computed with the mixing length parameter, α_MLT = 5.46. Similar to Fig. 3, a density inversion can be seen in panel (c). However, higher convective velocity (panel f) and smaller superadiabaticity (panel g) resulting from the higher value of α_MLT helps to keep the specific entropy small (panel d) and time steps large enough to evolve the model without numerical instabilities.