  Massive stars present strong stellar that which are described by the
radiation driven wind theory. Accurate mass-loss rates are necessary to
properly describe the stellar evolution across the Hertzsprung--Russel Diagram.
  We present a self-consistent procedure that coupled the hydrodynamics with
calculations of the line-force, giving as results the line-force parameters,
the velocity field, and the mass-loss rate. Our calculations contemplate the
contribution to the line-force multiplier from more than $\sim 900,000$ atomic
transitions, an NLTE radiation flux from the photosphere and a quasi-LTE
approximation for the occupational numbers.
  A full set of line-force parameters for $T_\text{eff}\ge 32,000$ K, surface
gravities higher than 3.4 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 empirical
values shows a good agreement. Self-consistent wind solutions are used as input
in FASTWIND to calculate synthetic spectra. We show, comparing with the
observed spectra for three stars, that 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.
