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To date, modern three-dimensional (3D) supernova (SN) simulations have notdemonstrated that explosion energies of 10^{51} erg (=1 bethe = 1B) or more arepossible for neutrino-driven SNe of non/slow-rotating M < 20 solar-massprogenitors. We present the first such model, considering a non-rotating,solar-metallicity 18.88 solar-mass progenitor, whose final 7 minutes ofconvective oxygen-shell burning were simulated in 3D and showed a violentoxygen-neon shell merger prior to collapse. A large set of 3D SN-models wascomputed with the Prometheus-Vertex code, whose improved convergence of thetwo-moment equations with Boltzmann closure allows now to fully exploit theimplicit neutrino-transport treatment. Nuclear burning is treated with a23-species network. We vary the angular grid resolution and consider differentnuclear equations of state and muon formation in the proto-neutron star (PNS),which requires six-species transport with coupling of all neutrino flavorsacross all energy-momentum groups. Elaborate neutrino transport was applieduntil ~2 seconds after bounce. In one case the simulation was continued to >7seconds with an approximate treatment of neutrino effects that allows forseamless continuation without transients. A spherically symmetricneutrino-driven wind does not develop. Instead, accretion downflows to the PNSand outflows of neutrino-heated matter establish a monotonic rise of theexplosion energy until ~7 seconds post bounce, when the outgoing shock reachesabout 50,000 km and enters the He-layer. The converged value of the explosionenergy at infinity (with overburden subtracted) is roughly 1B and the ejected56Ni mass up to 0.087 solar masses, both within a few 10 percent of the SN1987A values. The final NS mass and kick are about 1.65 solar masses and over450 km/s, respectively.

Self-consistent 3D Supernova Models From -7 Minutes to +7 Seconds: a 1-bethe Explosion of a ~19 Solar-mass Progenitor