The Boltzmann-radiation-hydrodynamics simulations of the core-collapse supernova with the different equations of state: The role of nuclear composition and the behavior of neutrinos

Akira Harada, Hiroki Nagakura, Wakana Iwakami, Hirotada Okawa, Shun Furusawa, Kohsuke Sumiyoshi, Hideo Matsufuru, Shoichi Yamada

Research output: Contribution to journalArticlepeer-review

Abstract

Using the Boltzmann-radiation-hydrodynamics code which solves the Boltzmann equation for the neutrino transport, we present the results of the simulations with the nuclear equations of state (EOSs) of Lattimer-Swesty (LS) and Furusawa-Shen (FS). We extend the simulation time of the LS model and conducted thorough investigations, though the previous paper reported some of the results briefly. Only the LS model shows the shock revival. This seems to originate from the nuclear composition: the different nuclear composition results in the different energy loss by the photodissociation and hence the different strength of the prompt convection and the later neutrino-driven convection. The proto-neutron star seen in the FS model is more compact than that in the LS model since the existence of multi-nuclear species softens the EOS. For the behavior of neutrinos, we examined the flux and the Eddington tensor of neutrinos. In the optically thick region, the diffusion of neutrinos and the dragging by the matter motion determine the flux. In the optically thin region, the free-streaming determines it. The Eddington tensor is compared with that obtained from the M1-closure relation. The M1-closure scheme overestimates the contribution from the velocity-dependent terms in the semitransparent region.

Original languageEnglish
JournalUnknown Journal
Publication statusPublished - 2020 Mar 19

Keywords

  • Equation of state
  • Methods: numerical
  • Neutrinos
  • Radiative transfer
  • Shock waves
  • Supernovae: general

ASJC Scopus subject areas

  • General

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