Evolutionary tracks, ejecta, and ionizing photons from intermediate-mass to very massive stars with PARSEC^⋆

¹ Dipartimento di Fisica e Astronomia, Università degli studi di Padova, Vicolo dell’Osservatorio 3, Padova, Italy
² Univ Lyon, Univ Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230 Saint-Genis-Laval, France
³ INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova, Italy
⁴ SISSA, Via Bonomea 365, I–34136 Trieste, Italy
⁵ Anhui University, Hefei 230601, China
⁶ Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
⁷ INAF – Osservatorio Astronomico di Trieste, Via Giambattista Tiepolo 11, Trieste, Italy
⁸ Dipartimento di Fisica e Astronomia Augusto Righi, Università degli Studi di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy

^⋆⋆ Corresponding authors; guglielmo.costa.astro@gmail.com, kshepher@sissa.it

Received: 11 October 2024
Accepted: 22 December 2024

Abstract

Recent advancements in stellar evolution modeling offer unprecedented accuracy in predicting the evolution and deaths of stars. We present new stellar evolutionary models computed with the updated PARSEC V2.0 code for a comprehensive and homogeneous grid of metallicities and initial masses. Nuclear reaction networks, mass loss prescriptions, and the treatment of elemental mixing have all been updated in PARSEC V2.0. We computed models for thirteen initial metallicities spanning Z = 10⁻¹¹ to Z = 0.03, with masses ranging from 2.0 M_⊙ to 2000 M_⊙, consisting of a library of over 1100 (∼2100 tracks including pure-He models) full stellar evolution tracks. For each track, the evolution is followed from the pre-main-sequence to the most advanced early-asymptotic-giant-branch or the pre-supernova phases (depending on the stellar mass). Here, we describe the properties of the tracks and their chemical and structural evolution. We computed the final fates and the remnant masses and built the mass spectrum for each metallicity, finding that the combined black hole (BH) pair-instability mass gap spans just between 100 and 130 M_⊙. Moreover, the remnant masses provide models consistent with observed BH masses, such as those from the primaries of GW190521, Cygnus X-1, and Gaia BH3 binary systems. We computed and provided the chemical ejecta from stellar winds and explosive final fates, along with the ionizing photon rates. We show how metallicity affects the evolution, fates, ejecta, and ionizing photon counts from these stars. Our results show strong overall consistency with other tracks computed with different codes, and the most significant discrepancies arise for very massive stars (M_ZAMS > 120 M_⊙) due to the different treatment of mixing and mass loss. A comparison with a large sample of observed massive stars in the Tarantula Nebula of the Large Magellanic Cloud shows that our tracks nicely reproduce the majority of stars that lie on the main sequence. All the models are publicly available and can be retrieved in the PARSEC database.