Self-consistent 3D Supernova Models From-7 Minutes to+7 s: A 1-bethe Explosion of a 19 M Progenitor

To date, modern three-dimensional (3D) supernova (SN) simulations have not demonstrated that explosion energies of 10(51) erg (=1 bethe=1 B) or more are possible for neutrino-driven SNe of non/slow-rotating M < 20 M (circle dot) progenitors. We present the first such model, considering a nonrotating, solar-metallicity 18.88 M (circle dot) progenitor, whose final 7 minutes of convective oxygen-shell burning were simulated in 3D and showed a violent oxygen-neon shell merger prior to collapse. A large set of 3D SN models was computed with the Prometheus-Vertex code, whose improved convergence of the two-moment equations with Boltzmann closure allows now to fully exploit the implicit neutrino-transport treatment. Nuclear burning is treated with a 23-species network. We vary the angular grid resolution and consider different nuclear equations of state and muon formation in the proto-neutron star (PNS), which requires six-species transport with coupling of all neutrino flavors across all energy-momentum groups. Elaborate neutrino transport was applied until similar to 2 s after bounce. In one case, the simulation was continued to >7 s with an approximate treatment of neutrino effects that allows for seamless continuation without transients. A spherically symmetric neutrino-driven wind does not develop. Instead, accretion downflows to the PNS and outflows of neutrino-heated matter establish a monotonic rise of the explosion energy until similar to 7 s post-bounce, when the outgoing shock reaches similar to 50,000 km and enters the He layer. The converged value of the explosion energy at infinity (with overburden subtracted) is similar to 1 B and the ejected Ni-56 mass less than or similar to 0.087 M (circle dot), both within a few 10% of the SN 1987A values. The final NS mass and kick are similar to 1.65 M (circle dot) and >450 km s(-1), respectively.