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

TL;DR

This paper presents the first 3D neutrino-driven supernova simulation of a ~19 solar-mass progenitor that successfully achieves an explosion energy of about 1 bethe, matching observed supernovae like SN 1987A.

Contribution

It demonstrates the feasibility of producing >10^{51} erg explosion energies in 3D simulations for non-rotating, solar-metallicity progenitors, using advanced neutrino transport and detailed physics.

Findings

Achieved a ~1 bethe explosion energy consistent with SN 1987A.

Ejected 56Ni mass up to 0.087 solar masses.

Final neutron star mass around 1.65 solar masses.

Abstract

To date, modern three-dimensional (3D) supernova (SN) simulations have not demonstrated that explosion energies of 10^{51} erg (=1 bethe = 1B) or more are possible for neutrino-driven SNe of non/slow-rotating M < 20 solar-mass progenitors. We present the first such model, considering a non-rotating, solar-metallicity 18.88 solar-mass 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 ~2 seconds after bounce. In one case the simulation was continued to >7 seconds 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 ~7 seconds post bounce, when the outgoing shock reaches about 50,000 km and enters the He-layer. The converged value of the explosion energy at infinity (with overburden subtracted) is roughly 1B and the ejected 56Ni mass up to 0.087 solar masses, both within a few 10 percent of the SN 1987A values. The final NS mass and kick are about 1.65 solar masses and over 450 km/s, respectively.