IR- and radio-fluxes from smooth and clumped wind models of wolf-rayet stars

Spherically-symmetric homogeneous (smooth) wind models predict smaller than the observed IR-fluxes and in many cases also smaller than the observed fluxes of HeI lines (in some cases also of HeII lines) if matter density is calibrated through the observed radio-fluxes. These discrepancies can be removed by clumped wind models. The mass loss rates determined for Wolf-Rayet stars by standard techniques through the radio-flux values seem to be the overestimates up to 1.1–2.5 times.