Three-dimensional simulation of a core-collapse supernova for a binary star progenitor of SN 1987A

Abstract

ABSTRACT We present results from a self-consistent, non-rotating core-collapse supernova simulation in three spatial dimensions using a binary evolution progenitor model of SN 1987A. This $18.3\, \mathrm{M}_{\odot }$ progenitor model is evolved from a slow merger of 14 and $9\, \mathrm{M}_{\odot }$ stars, and it satisfies most of the observational constraints such as red-to-blue evolution, lifetime, total mass, and position in the Hertzsprung–Russell diagram at collapse, and chemical anomalies. Our simulation is initiated from a spherically symmetric collapse and mapped to the three-dimensional coordinates at 10 ms after bounce to follow the non-spherical hydrodynamics evolution. We obtain the neutrino-driven shock revival for this progenitor at ∼350 ms after bounce, leading to the formation of a newly born neutron star with average gravitational mass ${\sim} 1.35\, \mathrm{M}_{\odot }$ and spin period ∼0.1 s. We also discuss the detectability of gravitational wave and neutrino signals for a Galactic event with the same characteristics as SN 1987A. At our final simulation time (∼660 ms post-bounce), the diagnostic explosion energy, though still growing, is smaller (0.14 foe) compared to the observed value (1.5 foe). The 56Ni mass obtained from the simulation ($0.01\, \mathrm{M}_{\odot }$) is also smaller than the reported mass from SN 1987A ($0.07\, \mathrm{M}_{\odot }$). Long-term simulation including several missing physical ingredients in our three-dimensional models such as rotation, magnetic fields, or more elaborate neutrino opacities should be done to bridge the gap between the theoretical predictions and the observed values.