Evolution of massive stars with new hydrodynamic wind models

Abstract

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 $120M_{\odot }$ 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 $a\sim 0.53$ when $M_{\ast }\sim 120M_{\odot }$, to $a\sim 1.02$ when $M_{\ast }\sim 25M_{\odot }$. 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 $\sim 0.1$ 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.

Accepted for publication in Astronomy & Astrophysics

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Cited by in corpus (1)

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