A successful 3D core-collapse supernova explosion model

Abstract

In this paper, we present the results of our three-dimensional, multigroup, multineutrino- species radiation/hydrodynamic simulation using the state-of-the-art code FORNAX of the terminal dynamics of the core of a non-rotating 16 M stellar progenitor. The calculation incorporates redistribution by inelastic scattering, a correction for the effect of many-body in- teractions on the neutrino–nucleon scattering rates, approximate general relativity (including the effects of gravitational redshifts), velocity-dependent frequency advection, and an imple- mentation of initial perturbations in the progenitor core. The model explodes within ∼ 100 ms of bounce (near when the silicon–oxygen interface is accreted through the temporarily stalled shock) and by the end of the simulation (here, ∼ 677 ms after bounce) is accumulating explo- sion energy at a rate of ∼ 2.5 × 10 50 erg s − 1 . The supernova explodes with an asymmetrical multiplume structure, with one hemisphere predominating. The gravitational mass of the resid- ual proto-neutron star at ∼ 677 ms is ∼ 1.42 M . Even at the end of the simulation, explosion in most of the solid angle is accompanied by some accretion in an annular region at the wasp-like waist of the debris field. The ejecta electron fraction ( Y e ) is distributed between ∼ 0.48 and ∼ 0.56, with most of the ejecta mass proton-rich. This may have implications for supernova nucleosynthesis, and could have a bearing on the p- and ν p-processes and on the site of the first peak of the r-process. The ejecta spatial distributions of both Y e and mass density are predominantly in wide-angle plumes and large-scale structures, but are nevertheless quite patchy.