TY - JOUR

T1 - Tables of hyperonic matter equation of state for core-collapse supernovae

AU - Ishizuka, Chikako

AU - Ohnishi, Akira

AU - Tsubakihara, Kohsuke

AU - Sumiyoshi, Kohsuke

AU - Yamada, Shoichi

N1 - Copyright:
Copyright 2015 Elsevier B.V., All rights reserved.

PY - 2008/8/1

Y1 - 2008/8/1

N2 - We present sets of equation of state (EOS) of nuclear matter including hyperons using an SUf(3) extended relativistic mean field (RMF) model with a wide coverage of density, temperature and charge fraction for numerical simulations of core-collapse supernovae. Coupling constants of Σ and Ξ hyperons with the σ meson are determined to fit the hyperon potential depths in nuclear matter, UΣ(ρ0) ≃ +30 MeV and UΞ(ρ0) ≃ -15 MeV, which are suggested from recent analyses of hyperon production reactions. At low densities, the EOS of uniform matter is connected with the EOS by Shen et al, in which the formation of finite nuclei is included in the Thomas-Fermi approximation. In the present EOS, the maximum mass of neutron stars decreases from 2.17 M⊙ (Neμ) to 1.63 M⊙ (NYeμ) when hyperons are included. In a spherical, adiabatic collapse of a 15 M⊙ star by the hydrodynamics without neutrino transfer, hyperon effects are found to be small, since the temperature and density do not reach the region of hyperon mixture, where the hyperon fraction is above 1 % (T > 40 MeV or ρB > 0.4 fm-3).

AB - We present sets of equation of state (EOS) of nuclear matter including hyperons using an SUf(3) extended relativistic mean field (RMF) model with a wide coverage of density, temperature and charge fraction for numerical simulations of core-collapse supernovae. Coupling constants of Σ and Ξ hyperons with the σ meson are determined to fit the hyperon potential depths in nuclear matter, UΣ(ρ0) ≃ +30 MeV and UΞ(ρ0) ≃ -15 MeV, which are suggested from recent analyses of hyperon production reactions. At low densities, the EOS of uniform matter is connected with the EOS by Shen et al, in which the formation of finite nuclei is included in the Thomas-Fermi approximation. In the present EOS, the maximum mass of neutron stars decreases from 2.17 M⊙ (Neμ) to 1.63 M⊙ (NYeμ) when hyperons are included. In a spherical, adiabatic collapse of a 15 M⊙ star by the hydrodynamics without neutrino transfer, hyperon effects are found to be small, since the temperature and density do not reach the region of hyperon mixture, where the hyperon fraction is above 1 % (T > 40 MeV or ρB > 0.4 fm-3).

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U2 - 10.1088/0954-3899/35/8/085201

DO - 10.1088/0954-3899/35/8/085201

M3 - Article

AN - SCOPUS:49749093034

SN - 0954-3899

VL - 35

JO - Journal of Physics G: Nuclear and Particle Physics

JF - Journal of Physics G: Nuclear and Particle Physics

IS - 8

M1 - 085201

ER -