From supernovae to neutron stars

Understand

The gravitational collapse, bounce, the explosion of an iron core of an 11.2 $M_{\odot}$ star is simulated by two-dimensional neutrino-radiation hydrodynamic code.

• The explosion is driven by the neutrino heating aided by multi-dimensional hydrodynamic effects such as the convection.
• Following the explosion phase, we continue the simulation focusing on the thermal evolution of the protoneutron star up to $\sim$70 s when the crust of the neutron star is formed using one-dimensional simulation.
• We find that the crust forms at high-density region ($\rho\sim10^{14}$ g cm$^{-3}$) and it would proceed from inside to outside.