  We perform spectral fitting for a set of O-type stars based on
self-consistent wind solutions, which provide mass-loss rate and velocity
profiles directly derived from the initial stellar parameters. The great
advantage of this self-consistent spectral fitting is therefore the reduction
of the number of free parameters to be tuned.
  Self-consistent values for the line-force parameters (k,alpha,delta) and
subsequently for the mass-loss rate and terminal velocity are provided by the
m-CAK prescription introduced in Paper I, updated in this work with
improvements such as a temperature structure for the wind, self-consistently
evaluated from the line-acceleration. Synthetic spectra are calculated using
the radiative transfer code FASTWIND, replacing the classical beta-law for our
new calculated velocity profiles.
  We found that self-consistent m-CAK solutions provide values for theoretical
mass-loss rates on the order of the most recent predictions of other studies.
From here, we generate synthetic spectra with self-consistent hydrodynamics to
fit and obtain a new set of stellar and wind parameters for our sample of
O-type stars whose spectra was taken with the high resolution echelle
spectrograph HERMES (R=85000). We find a satisfactory global fit for our
observations, with good accuracy for photospheric He I and He II lines and a
quite acceptable fit for H lines. Although this self-consistent spectral
analysis is currently constrained in the optical wavelength range only, this is
an important step towards the determination of stellar and wind parameters
without using a beta-law. Given these results, we expect that the values
introduced here should be helpful for future studies about the stars
constituting this sample, together with the prospective that the m-CAK
self-consistent prescription be extended to numerous studies about massive
stars in future.
