Three-dimensional Hydrodynamic Core-Collapse Supernova Simulations for an $11.2 M_{\odot}$ Star with Spectral Neutrino Transport

TL;DR

This study presents 3D hydrodynamic simulations of an 11.2 solar mass star's core-collapse supernova, highlighting how 3D effects influence explosion dynamics, neutrino emission, and the importance of numerical resolution.

Contribution

First 3D simulations of an 11.2 M_sun star with spectral neutrino transport, analyzing multi-dimensional effects on supernova explosion mechanisms.

Findings

3D models show longer residency times in the gain region due to non-axisymmetric flows.

Convective motions below the gain radius are more violent in 3D, increasing neutrino luminosity.

Shock energy increases with higher numerical resolution in 3D simulations.

Abstract

We present numerical results on three-dimensional (3D) hydrodynamic core-collapse simulations of an $11.2 M_{\odot}$ star. By comparing one-(1D) and two-dimensional(2D) results with those of 3D, we study how the increasing spacial multi-dimensionality affects the postbounce supernova dynamics. The calculations were performed with an energy-dependent treatment of the neutrino transport that is solved by the isotropic diffusion source approximation scheme. By performing a tracer-particle analysis, we show that the maximum residency time of material in the gain region is shown to be longer for 3D due to non-axisymmetric flow motions than 2D, which is one of advantageous aspects of 3D models to obtain neutrino-driven explosions. Our results show that convective matter motions below the gain radius become much more violent in 3D than 2D, making the neutrino luminosity larger for 3D. Nevertheless the emitted neutrino energies are made smaller due to the enhanced cooling. Our results indicate whether these advantages for driving 3D explosions could or could not overwhelm the disadvantages is sensitive to the employed numerical resolutions. An encouraging finding is that the shock expansion tends to become more energetic for models with finer resolutions. To draw a robust conclusion, 3D simulations with much more higher numerical resolutions and also with more advanced treatment of neutrino transport as well as of gravity is needed, which could be hopefully practicable by utilizing forthcoming Petaflops-class supercomputers.