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

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 M-circle dot progenitor model is evolved from a slow merger of 14 and 9 M-circle dot 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 similar to 350 ms after bounce, leading to the formation of a newly born neutron star with average gravitational mass similar to 1.35M(circle dot) and spin period similar to 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 (similar to 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 Ni-56 mass obtained from the simulation (0.01M(circle dot)) is also smaller than the reported mass from SN 1987A (0.07 M-circle dot). 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.