学术文献库

A crucial ingredient in population synthesis studies involving massive stars is the determination of whether they explode or implode in the end. While the final fate of a massive star is sensitive to its core structure at the onset of collapse, the existing binary population synthesis studies do not reach core-collapse. Instead, they employ simple prescriptions to infer their final fates without knowing the presupernova core structure. We explore a potential solution to this problem by treating the carbon-oxygen (CO) core independently from the rest of the star. Using the implicit hydrodynamics code KEPLER, we have computed an extensive grid of 3496 CO-core models from a diverse range of initial conditions, each evolved from carbon ignition until core-collapse. The final core structure, and thus the explodability, varies non-monotonically and depends sensitively on both the mass and initial composition of the CO-core. Although bare CO-cores are not perfect substitutes for cores embedded in massive stars, our models compare well both with MESA and full hydrogenic and helium star calculations. Our results can be used to infer the presupernova core structures from population synthesis estimates of CO-core properties, thus to determine the final outcomes based on the results of modern neutrino-driven explosion simulations. A sample application is presented for a population of Type-IIb supernova progenitors. All of our models are available at https://doi.org/10.5281/zenodo.3785377.