From supernovae to neutron stars

Gravitational collapse, bounce, and explosion of an iron core of an 11.2 M⊙ star are simulated by two-dimensional neutrino-radiation hydrodynamic code. The explosion is driven by the neutrino heating aided by multi-dimensional hydrodynamic effects such as convection. Following the explosion phase, we continue the simulation focusing on the thermal evolution of the protoneutron star up to ∼ 70 s when the crust of the neutron star is formed, using one-dimensional simulation. We find that the crust forms at a high-density region (ρ ∼ 1014 g cm−3) and it proceeds from inside to outside. This is the first self-consistent simulation that successfully follows from the collapse phase to the protoneutron star cooling phase based on multi-dimensional hydrodynamic simulation.