Non-LTE iron blanketed model atmospheres are calculated with the new Potsdam code for expanding atmospheres. A blanketed model for the early WC star WR 111 is compared to its unblanketed counterpart. The resulting effects on the ionization and temperature structure are discussed. In the optically thick part of the envelope a higher temperature is obtained through the back warming effect of the additional opacities. In the outer part the recombination from He III to He II, from C IV to C III and from O IV to O III is considerably enhanced. This leads to a broader range of apparent ionic species in the model spectrum. Additionally the blanketed model provides a force by radiation pressure which supplies a considerable amount of the wind acceleration.