Pulsational pair-instability supernovae: gravitational collapse, black hole formation, and beyond

We investigate the final collapse of rotating and non-rotating pulsational pair-instability supernova progenitors with zero-age-main-sequence masses 60, 80, 115$\mathrm{M}_\odot$ iron cores between 2.37$\mathrm{M}_\odot$ 2.72$\mathrm{M}_\odot$ by 2D hydrodynamics simulations. Using general relativistic NADA-FLD code energy-dependent three-flavor neutrino transport flux-limited diffusion allows us to follow evolution beyond moment when transiently forming neutron star (NS) collapses a black hole (BH), which happens within 350$-$580 ms after bounce in all cases. Because high luminosities mean energies, heating leads shock revival $\lesssim$250 post cases except rapidly 60$\mathrm{M}_\odot$ model. In latter case, centrifugal effects support 10% higher NS mass but reduce radiated energies $\sim$20% $\sim$10%, respectively, neutrino-heating rate roughly factor two compared counterpart. After BH formation, drop steeply continue on 1$-$2 orders magnitude lower level for several 100 because aspherical accretion shock-heated matter, before ultimately spherical outer progenitor shells suppresses emission negligible values. shock-reviving models swallows entire neutrino-heated matter explosion decrease from maxima around 1.5$\times$10$^{51}$erg zero few seconds latest. Nevertheless, or sonic pulse moves outward may trigger loss, we estimate long-time simulations PROMETHEUS code. also provide gravitational-wave signals.