Evolution of massive stars with new hydrodynamic wind models

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