Black Hole Supernovae, their Equation of State Dependence and Ejecta Composition

Recent literature on core-collapse supernovae suggests that a black hole (BH) can form within \(\sim 1\) s of shock revival, while still culminating in a successful supernova. We refer to these as black hole supernovae, as they are distinct from other BH formation channels in both timescale and impact on the explosion. We simulate these events self-consistently from core-collapse until \(20\text{-}50\) days after collapse using three axisymmetric models of a \(60\) M\(_\odot\) zero-age main sequence progenitor star and investigate how the composition of the ejecta is impacted by the BH formation. We employ Skyrme-type equations of state (EOSs) and vary the uncertain nucleonic effective mass, which affects the pressure inside the proto-neutron star through the thermal part of the EOS. This results in different BH formation times and explosion energies at BH formation, yielding final explosion energies between \(0.06\text{-}0.72\times 10^{51}\) erg with \(21.8\text{-}23.3\) M\(_\odot\) of ejecta, of which \(0\text{-}0.018\) M\(_\odot\) is \(^{56}\)Ni. Compared to expectations from 1D simulations, we find a more nuanced EOS dependence of the explosion dynamics, the mass of the BH remnant, and the elemental composition of the ejecta. We investigate why the explosions survive despite the massive overburden and link the shape of the diagnostic energy curve and character of the ejecta evolution to the progenitor structure.