Chikako Ishizuka et al 2008 J. Phys. G: Nucl. Part. Phys. 35 085201 doi:10.1088/0954-3899/35/8/085201
Tables of hyperonic matter equation of state for core-collapse supernovae*
Chikako Ishizuka1, Akira Ohnishi1,2, Kohsuke Tsubakihara1, Kohsuke Sumiyoshi3 and Shoichi Yamada4
Show affiliationsWe 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).
- Footnote
- PACS
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97.10.Cv Stellar structure, interiors, evolution, nucleosynthesis, ages
95.30.Cq Elementary particle processes
26.50.+x Nuclear physics aspects of novae, supernovae, and other explosive environments
95.30.Tg Thermodynamic processes, conduction, convection, equations of state
- Subjects
- Dates
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Issue 8 (August 2008)
Received 16 February 2008
Published 8 July 2008
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Tables of hyperonic matter equation of state for core-collapse supernovae
Chikako Ishizuka et al 2008 J. Phys. G: Nucl. Part. Phys. 35 085201
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