2024MNRAS.529..178C

We perform a set of two-dimensional, non-relativistic, hydrodynamics simulations for supernova-like explosions associated with stellar core collapse of rotating massive stars into a system of a black hole and a disc connected by the transfer of matter and angular momentum. Our model of the central engine also includes the contribution of the disc wind. This study is carried out using the open-source hydrodynamic code ATHENA++, for which we implement a method to calculate self-gravity for axially symmetric density distributions. We investigate the explosion properties and the ⁵⁶Ni production of a star with the zero-age main-sequence mass of $M_\mathrm{ZAMS}=20\, M_\odot$ varying some features of the wind injection. We find a large variety of explosion energy with E_expl ranging from ∼0.049 × 10⁵¹ to ∼34 × 10⁵¹ erg and ejecta mass M_ej from 0.58 to 6 M_⊙, which shows a bimodal distribution in high- and low-energy branches. We demonstrate that the resulting outcome of a highly or sub-energetic explosion for a certain stellar structure is mainly determined by the competition between the ram pressure of the injected matter and that of the infalling envelope. In the nucleosynthesis analysis the ⁵⁶Ni mass produced in our models goes from <0.2 M_⊙ in the sub-energetic explosions to 2.1 M_⊙ in the highly energetic ones. These results are consistent with the observational data of stripped-envelope and high-energy SNe such as broad-lined Type Ic SNe.