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We provide hot star wind models with radiative force calculated using thesolution of comoving frame (CMF) radiative transfer equation. The wind modelsare calculated for the first stars, O stars, and the central stars of planetarynebulae. We show that without line overlaps and with solely thermal linebroadening the pure Sobolev approximation provides a reliable estimate of theradiative force even close to the wind sonic point. Consequently, models withthe Sobolev line force provide good approximations to solutions obtained withnon-Sobolev transfer. Taking line overlaps into account, the radiative forcebecomes slightly lower, leading to a decrease in the wind mass-loss rate byroughly 40%. Below the sonic point, the CMF line force is significantly lowerthan the Sobolev one. In the case of pure thermal broadening, this does notinfluence the mass-loss rate, as the wind mass-loss rate is set in thesupersonic part of the wind. However, when additional line broadening ispresent (e.g., the turbulent one) the region of low CMF line force may extendoutwards to the regions where the mass-loss rate is set. This results in adecrease in the wind mass-loss rate. This effect can at least partly explainthe low wind mass-loss rates derived from some observational analyses ofluminous O stars.

CMF models of hot star winds I. Test of the Sobolev approximation in the case of pure line transitions