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

^*この研究の対応する著者

先進理工学部

研究成果: Article › 査読

40 被引用数 (Scopus)

抄録

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.

本文言語	English
ページ（範囲）	232-250
ページ数	19
ジャーナル	Nuclear Physics A
巻	791
号	1-2
DOI	https://doi.org/10.1016/j.nuclphysa.2007.01.098
出版ステータス	Published - 2007 7月 1

ASJC Scopus subject areas

核物理学および高エネルギー物理学

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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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T1 - Variational calculation for the equation of state of nuclear matter at finite temperatures

AU - Kanzawa, H.

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

Y1 - 2007/7/1

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.

KW - Neutron stars

KW - Nuclear EOS

KW - Nuclear matter

KW - Supernovae

KW - Variational method

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

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