Evolving massive stars to core collapse with GENEC: Extension of equation of state, opacities and effective nuclear network

¹ Departament d’Astonomia i Astrofísica, Universitat de València, C/Dr. Moliner, 50, E-46100 Burjassot, València, Spain
² Observatori Astronòmic, Universitat de València, 46980 Paterna, Spain
³ Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UK
⁴ Kavli IPMU (WPI), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa 277-8583, Japan
⁵ Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles (ULB), CP 226, B-1050 Brussels, Belgium
⁶ Geneva Observatory, University of Geneva, Chemin Pegasi 51, CH-1290 Sauverny, Switzerland

^⋆ Corresponding authors; adam.griffiths@uv.es, miguel.a.aloy@uv.es

Received: 6 August 2024
Accepted: 26 November 2024

Abstract

Context. Stars with initial mass above roughly 8 M_⊙ will evolve to form a core made of iron group elements, at which point no further exothermic nuclear reactions between charged nuclei may prevent the core collapse. Electron capture, neutrino losses, and the photo-disintegration of heavy nuclei trigger the collapse of these stars. Models at the brink of core collapse are produced using stellar evolution codes, and these pre-collapse models may be used in the study of the subsequent dynamical evolution (including their explosion as supernovae and the formation of compact remnants such as neutron stars or black holes).

Aims. We upgraded the physical ingredients employed by the GENeva stellar Evolution Code, GENEC, so that it covers the regime of high-temperatures and high-densities required to produce the progenitors of core-collapse. Our ultimate goal is producing pre-supernova models with GENEC, not only right before collapse, but also during the late phases (silicon and oxygen burning).

Methods. We have improved GENEC in three directions: equation of state, the nuclear reaction network, and the radiative and conductive opacities adapted for the computation of the advanced phases of evolution. We produce a small grid of pre-supernova models of stars with zero age main sequence masses of 15 M_⊙, 20 M_⊙, and 25 M_⊙ at solar and less than half solar metallicities. The results are compared with analogous models produced with the MESA code.

Results. The global properties of our new models, particularly of their inner cores, are comparable to models computed with MESA and pre-existing progenitors in the literature. Between codes the exact shell structure varies, and impacts explosion predictions.

Conclusions. Using GENEC with state-of-the-art physics, we have produced massive stellar progenitors prior to collapse. These progenitors are suitable for follow-up studies, including the dynamical collapse and supernova phases. Larger grids of supernova progenitors are now feasible, with the potential for further dynamical evolution.