From supernovae to neutron stars

Abstract

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 \sim 10^{14}$ g cm${}^{-3}$) 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.

5 pages, 3 figures, with minor corrections; accepted to PASJ Letters

References in corpus (8)

• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• Delayed neutrino-driven supernova explosions aided by the standing accretion-shock instability
• The Breaking Strain of Neutron Star Crust and Gravitational Waves
• The isotropic diffusion source approximation for supernova neutrino transport
• Phase separation in the crust of accreting neutron stars
• A Mathematical Description of the IDSA for Supernova Neutrino transport, its discretization and a comparison with a finite volume scheme for Boltzmann's Equation
• Comment on ``Symplectic quantization, inequivalent quantum theories, and Heisenberg's principle of uncertainty''

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