  Here we present evolutionary models for a set of massive stars, introducing a
new prescription for the mass-loss rate obtained from hydrodynamical
calculations in which the wind velocity profile, $v(r)$, and the
line-acceleration, $g_\text{line}$, are obtained in a self consistently way.
Replacing mass-loss rates at the Main Sequence stage from the standard Vink's
formula by our new recipe, we generate a new set of evolutionary tracks for
$M_\text{ZAMS}=25,40,70$ and $120\,M_\odot$ and metallicities $Z=0.014$
(Galactic), $Z=0.006$ (LMC), and $Z=0.002$ (SMC).
  Our new derived formula for mass-loss rate predicts a dependence $\dot
M\propto Z^a$, where $a$ is not longer constant but dependent on the stellar
mass: ranging from $a\sim0.53$ when $M_*\sim120\;M_\odot$, to $a\sim1.02$ when
$M_*\sim25\;M_\odot$.
  We found that models adopting the new recipe for $\dot M$ retain more mass
during their evolution, which is expressed in larger radii and consequently
more luminous tracks over the Hertzsprung-Russell diagram. These differences
are more prominent for the cases of $M_\text{ZAMS}=70$ and 120 $M_\odot$ at
solar metallicity, where we found self-consistent tracks are $\sim0.1$ dex
brighter and keep extra mass up to 20 $M_\odot$, compared with the classical
models using the previous formulation for mass-loss rate.
  Moreover, we observed remarkable differences for the evolution of the
radionuclide isotope $^{26}$Al in the core and the surface of the star. Since
$\dot M_\text{sc}$ are weaker than the commonly adopted values for evolutionary
tracks, self-consistent tracks predict a later modification in the abundance
number of $^{26}$Al in the stellar winds. This new behaviour could provide
useful information about the real contribution of this isotope from massive
stars to the Galactic interstellar medium.
