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From supernovae to neutron stars
The gravitational collapse, bounce, the explosion of an iron core of an 11.2
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 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 ( g cm) and it would proceed 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 the multi-dimensional hydrodynamic simulation.Comment: 5 pages, 3 figures, with minor corrections; accepted to PASJ Letter
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