Variational calculation for the equation of state of nuclear matter at finite temperatures

H. Kanzawa; K. Oyamatsu; K. Sumiyoshi; M. Takano

doi:10.1016/j.nuclphysa.2007.01.098

Variational calculation for the equation of state of nuclear matter at finite temperatures

H. Kanzawa^*, K. Oyamatsu, K. Sumiyoshi, M. Takano

^*Corresponding author for this work

School of Advanced Science and Engineering

Research output: Contribution to journal › Article › peer-review

42 Citations (Scopus)

Abstract

An equation of state (EOS) for uniform nuclear matter is constructed at zero and finite temperatures with the variational method starting from the realistic nuclear Hamiltonian composed of the Argonne V18 and UIX potentials. The energy is evaluated in the two-body cluster approximation with the three-body-force contribution treated phenomenologically so as to reproduce the empirical saturation conditions. The obtained energies for symmetric nuclear matter and neutron matter at zero temperature are in fair agreement with those by Akmal, Pandharipande and Ravenhall, and the maximum mass of the neutron star is 2.2 M_ȯ. At finite temperatures, a variational method by Schmidt and Pandharipande is employed to evaluate the free energy, which is used to derive various thermodynamic quantities of nuclear matter necessary for supernova simulations. The result of this variational method at finite temperatures is found to be self-consistent.

Original language	English
Pages (from-to)	232-250
Number of pages	19
Journal	Nuclear Physics A
Volume	791
Issue number	1-2
DOIs	https://doi.org/10.1016/j.nuclphysa.2007.01.098
Publication status	Published - 2007 Jul 1

Keywords

Neutron stars
Nuclear EOS
Nuclear matter
Supernovae
Variational method

ASJC Scopus subject areas

Nuclear and High Energy Physics

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10.1016/j.nuclphysa.2007.01.098

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title = "Variational calculation for the equation of state of nuclear matter at finite temperatures",

abstract = "An equation of state (EOS) for uniform nuclear matter is constructed at zero and finite temperatures with the variational method starting from the realistic nuclear Hamiltonian composed of the Argonne V18 and UIX potentials. The energy is evaluated in the two-body cluster approximation with the three-body-force contribution treated phenomenologically so as to reproduce the empirical saturation conditions. The obtained energies for symmetric nuclear matter and neutron matter at zero temperature are in fair agreement with those by Akmal, Pandharipande and Ravenhall, and the maximum mass of the neutron star is 2.2 Mȯ. At finite temperatures, a variational method by Schmidt and Pandharipande is employed to evaluate the free energy, which is used to derive various thermodynamic quantities of nuclear matter necessary for supernova simulations. The result of this variational method at finite temperatures is found to be self-consistent.",

keywords = "Neutron stars, Nuclear EOS, Nuclear matter, Supernovae, Variational method",

author = "H. Kanzawa and K. Oyamatsu and K. Sumiyoshi and M. Takano",

note = "Funding Information: We would like to express special thanks to Profs. S. Yamada, M. Yamada and K. Iida for valuable discussions. We also appreciate the cooperation of Messrs. K. Tanaka and K. Murai received in the early stage of this study. This study is supported by a Grant-in-Aid for the 21st century COE program “Holistic Research and Education Center for Physics of Self-organizing Systems” at Waseda University, and Grants-in-Aid from the Scientific Research Fund of the JSPS (Nos. 15540243, 18540291 and 18540295). Some of the numerical calculations were performed with a SR8000/MPP at the Information Technology Center of the University of Tokyo.",

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AU - Oyamatsu, K.

AU - Sumiyoshi, K.

AU - Takano, M.

N1 - Funding Information: We would like to express special thanks to Profs. S. Yamada, M. Yamada and K. Iida for valuable discussions. We also appreciate the cooperation of Messrs. K. Tanaka and K. Murai received in the early stage of this study. This study is supported by a Grant-in-Aid for the 21st century COE program “Holistic Research and Education Center for Physics of Self-organizing Systems” at Waseda University, and Grants-in-Aid from the Scientific Research Fund of the JSPS (Nos. 15540243, 18540291 and 18540295). Some of the numerical calculations were performed with a SR8000/MPP at the Information Technology Center of the University of Tokyo.

PY - 2007/7/1

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N2 - An equation of state (EOS) for uniform nuclear matter is constructed at zero and finite temperatures with the variational method starting from the realistic nuclear Hamiltonian composed of the Argonne V18 and UIX potentials. The energy is evaluated in the two-body cluster approximation with the three-body-force contribution treated phenomenologically so as to reproduce the empirical saturation conditions. The obtained energies for symmetric nuclear matter and neutron matter at zero temperature are in fair agreement with those by Akmal, Pandharipande and Ravenhall, and the maximum mass of the neutron star is 2.2 Mȯ. At finite temperatures, a variational method by Schmidt and Pandharipande is employed to evaluate the free energy, which is used to derive various thermodynamic quantities of nuclear matter necessary for supernova simulations. The result of this variational method at finite temperatures is found to be self-consistent.

AB - An equation of state (EOS) for uniform nuclear matter is constructed at zero and finite temperatures with the variational method starting from the realistic nuclear Hamiltonian composed of the Argonne V18 and UIX potentials. The energy is evaluated in the two-body cluster approximation with the three-body-force contribution treated phenomenologically so as to reproduce the empirical saturation conditions. The obtained energies for symmetric nuclear matter and neutron matter at zero temperature are in fair agreement with those by Akmal, Pandharipande and Ravenhall, and the maximum mass of the neutron star is 2.2 Mȯ. At finite temperatures, a variational method by Schmidt and Pandharipande is employed to evaluate the free energy, which is used to derive various thermodynamic quantities of nuclear matter necessary for supernova simulations. The result of this variational method at finite temperatures is found to be self-consistent.

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KW - Nuclear EOS

KW - Nuclear matter

KW - Supernovae

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Variational calculation for the equation of state of nuclear matter at finite temperatures

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