Massive stars present strong stellar winds that are described by the m-CAK radiation driven wind theory. We present a novel self-consistent procedure that couples the hydrodynamics with calculations of the line-force, giving as result the line-force parameters, the velocity field, and the mass-loss rate. Our calculations take into account: the contribution to the line-force multiplier from more than ~900,000 atomic transitions, an NLTE radiation flux from the photosphere from Tlusty models and a quasi-LTE approximation for the occupational numbers. A full set of line-force parameters for T_eff ≥ 30,000 K, surface gravities higher than 3.2 dex for two different metallicities are presented, with their corresponding wind parameters (terminal velocities and mass-loss rates). The already known dependence of line-force parameters on effective temperature is enhanced by the dependence on log g. The terminal velocities present a stepper scaling relation with respect to the escape velocity, this might explain the scatter values observed in the hot side of the bistability jump. Moreover, a comparison of self-consistent mass-loss rates with the one obtained by the m-CAK theory shows a good agreement, but with a difference in the mass-loss rates of a factor > 2. Self-consistent wind solutions are used as input in FASTWIND and CMFGEN to calculate synthetic spectra. We show, comparing with the observed spectra for some stars, that only varying the clumping factor, the synthetic spectra rapidly converge into the neighbourhood region of the solution. It is important to stress that our self-consistent procedure significantly reduces the number of free parameters needed to obtain a synthetic spectrum.