### Abstract

A new table of the nuclear equation of state (EOS) based on realistic nuclear potentials is constructed for core-collapse supernova numerical simulations. Adopting the EOS of uniform nuclear matter constructed by two of the present authors with the cluster variational method starting from the Argonne v18 and Urbana IX nuclear potentials, the Thomas–Fermi calculation is performed to obtain the minimized free energy of a Wigner–Seitz cell in non-uniform nuclear matter. As a preparation for the Thomas–Fermi calculation, the EOS of uniform nuclear matter is modified so as to remove the effects of deuteron cluster formation in uniform matter at low densities. Mixing of alpha particles is also taken into account following the procedure used by Shen et al. (1998, 2011). The critical densities with respect to the phase transition from non-uniform to uniform phase with the present EOS are slightly higher than those with the Shen EOS at small proton fractions. The critical temperature with respect to the liquid–gas phase transition decreases with the proton fraction in a more gradual manner than in the Shen EOS. Furthermore, the mass and proton numbers of nuclides appearing in non-uniform nuclear matter with small proton fractions are larger than those of the Shen EOS. These results are consequences of the fact that the density derivative coefficient of the symmetry energy of our EOS is smaller than that of the Shen EOS.

Original language | English |
---|---|

Pages (from-to) | 78-105 |

Number of pages | 28 |

Journal | Nuclear Physics A |

Volume | 961 |

DOIs | |

Publication status | Published - 2017 May 1 |

### Fingerprint

### Keywords

- Neutron stars
- Nuclear EOS
- Nuclear matter
- Supernovae
- Variational method

### ASJC Scopus subject areas

- Nuclear and High Energy Physics

### Cite this

*Nuclear Physics A*,

*961*, 78-105. https://doi.org/10.1016/j.nuclphysa.2017.02.010

**Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces.** / Togashi, H.; Nakazato, K.; Takehara, Y.; Yamamuro, S.; Suzuki, H.; Takano, Masatoshi.

Research output: Contribution to journal › Article

*Nuclear Physics A*, vol. 961, pp. 78-105. https://doi.org/10.1016/j.nuclphysa.2017.02.010

}

TY - JOUR

T1 - Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces

AU - Togashi, H.

AU - Nakazato, K.

AU - Takehara, Y.

AU - Yamamuro, S.

AU - Suzuki, H.

AU - Takano, Masatoshi

PY - 2017/5/1

Y1 - 2017/5/1

N2 - A new table of the nuclear equation of state (EOS) based on realistic nuclear potentials is constructed for core-collapse supernova numerical simulations. Adopting the EOS of uniform nuclear matter constructed by two of the present authors with the cluster variational method starting from the Argonne v18 and Urbana IX nuclear potentials, the Thomas–Fermi calculation is performed to obtain the minimized free energy of a Wigner–Seitz cell in non-uniform nuclear matter. As a preparation for the Thomas–Fermi calculation, the EOS of uniform nuclear matter is modified so as to remove the effects of deuteron cluster formation in uniform matter at low densities. Mixing of alpha particles is also taken into account following the procedure used by Shen et al. (1998, 2011). The critical densities with respect to the phase transition from non-uniform to uniform phase with the present EOS are slightly higher than those with the Shen EOS at small proton fractions. The critical temperature with respect to the liquid–gas phase transition decreases with the proton fraction in a more gradual manner than in the Shen EOS. Furthermore, the mass and proton numbers of nuclides appearing in non-uniform nuclear matter with small proton fractions are larger than those of the Shen EOS. These results are consequences of the fact that the density derivative coefficient of the symmetry energy of our EOS is smaller than that of the Shen EOS.

AB - A new table of the nuclear equation of state (EOS) based on realistic nuclear potentials is constructed for core-collapse supernova numerical simulations. Adopting the EOS of uniform nuclear matter constructed by two of the present authors with the cluster variational method starting from the Argonne v18 and Urbana IX nuclear potentials, the Thomas–Fermi calculation is performed to obtain the minimized free energy of a Wigner–Seitz cell in non-uniform nuclear matter. As a preparation for the Thomas–Fermi calculation, the EOS of uniform nuclear matter is modified so as to remove the effects of deuteron cluster formation in uniform matter at low densities. Mixing of alpha particles is also taken into account following the procedure used by Shen et al. (1998, 2011). The critical densities with respect to the phase transition from non-uniform to uniform phase with the present EOS are slightly higher than those with the Shen EOS at small proton fractions. The critical temperature with respect to the liquid–gas phase transition decreases with the proton fraction in a more gradual manner than in the Shen EOS. Furthermore, the mass and proton numbers of nuclides appearing in non-uniform nuclear matter with small proton fractions are larger than those of the Shen EOS. These results are consequences of the fact that the density derivative coefficient of the symmetry energy of our EOS is smaller than that of the Shen EOS.

KW - Neutron stars

KW - Nuclear EOS

KW - Nuclear matter

KW - Supernovae

KW - Variational method

UR - http://www.scopus.com/inward/record.url?scp=85014287771&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85014287771&partnerID=8YFLogxK

U2 - 10.1016/j.nuclphysa.2017.02.010

DO - 10.1016/j.nuclphysa.2017.02.010

M3 - Article

VL - 961

SP - 78

EP - 105

JO - Nuclear Physics A

JF - Nuclear Physics A

SN - 0375-9474

ER -