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, M.

N1 - Funding Information:
We would like to express special thanks to H. Kanzawa, K. Oyamatsu, K. Sumiyoshi, M. Yamada and S. Yamada for valuable discussions and comments, to H. Shen for providing us with numerical data on parameters for the Thomas–Fermi calculation, and to H. Matsufuru for supporting on parallel computing. Early stages of the healing-distance modification were performed by Y. Nagano. The numerical computations in this work were carried out on SR16000 at YITP in Kyoto University, on SR16000 and Blue Gene/Q at the High Energy Accelerator Research Organization (KEK), and on SR16000 at the Information Technology Center of the University of Tokyo. This work is supported by JSPS (Nos. 22540296, 23224006, 24244036, 25400275, 26870615), the Grant-in-Aid for Scientific Research on Innovative Areas of MEXT (Nos. 20105003, 20105004, 20105005, 24105008, 26104006, 26105515), RIKEN iTHES Project, and Special Postdoctoral Researcher Program of RIKEN.
Publisher Copyright:
© 2017 Elsevier B.V.

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.

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U2 - 10.1016/j.nuclphysa.2017.02.010

DO - 10.1016/j.nuclphysa.2017.02.010

M3 - Article

AN - SCOPUS:85014287771

VL - 961

SP - 78

EP - 105

JO - Nuclear Physics A

JF - Nuclear Physics A

SN - 0375-9474

ER -