A comprehensive grid of massive binary evolution models for the Galaxy: Surface properties of post-mass-transfer stars

Context. Massive stars often evolve in binary systems, and the interactions of these systems significantly affect their evolution. Massive stars in the Galaxy serve as valuable test beds for such interactions due to their proximity. Aims. We computed the evolution of more than 38 000 galactic binary systems with initial primary star masses of 5 − 100 M ⊙ . In this paper we aim to investigate the surface properties of post-mass-transfer mass donor and mass-gainer stars through core hydrogen burning, core helium burning, and for the pre-supernova stage. Methods. The models were computed with MESA, incorporating detailed stellar and binary physics, including internal differential rotation, magnetic angular momentum transport, mass-dependent overshooting, stellar wind mass-loss, mass and angular momentum transfer, and tidal interaction. They incorporate a new extensive nuclear network for hydrogen burning, which allow us to track the full range of hydrogen burning nucleosynthesis products, from the light elements to aluminum. The widest non-interacting binary models in our grid effectively serve as single-star models. Results. We find that mass gainers and donors may evolve through long-lived blue and yellow supergiant stages during core helium burning, where single stars of the same mass remain red supergiants. Furthermore, some of our mass gainers evolve into more luminous yellow and blue supergiants prior to core collapse than single stars, while some mass donors end their life as red or yellow supergiants, showing a rich diversity in supernova progenitors. We show that the surface elemental and isotopic abundances carry valuable information about a star’s evolutionary history and can be used to distinguish binary interaction products from single stars. Conclusions. Our binary model grid may serve as a tool for identifying post-mass-transfer stars and supernovae. It also holds potential for population studies, supernova modeling, and guidance of future observations.