### 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 AV18 two-body potential and the UIX three-body potential. The maximum mass of the cold neutron star with this EOS is 2.2 M
_{⊙}. Making use of uncertainty of the three-body nuclear force, adjustable parameters in the EOS are tuned so that the Thomas-Fermi calculations for β-stable nuclei reproduce the empirical data. The obtained EOS is appropriate for constructing a new nuclear EOS table for supernova simulations.

Original language | English |
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Title of host publication | Proceedings of Science |

Publication status | Published - 2008 |

Event | 10th Symposium on Nuclei in the Cosmos, NIC 2008 - Mackinac Island, MI, United States Duration: 2008 Jul 27 → 2008 Aug 1 |

### Other

Other | 10th Symposium on Nuclei in the Cosmos, NIC 2008 |
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Country | United States |

City | Mackinac Island, MI |

Period | 08/7/27 → 08/8/1 |

### Fingerprint

### ASJC Scopus subject areas

- General

### Cite this

*Proceedings of Science*

**Nuclear many-body approach for supernova EOS : Thomas-fermi calculations of non-uniform nuclear matter.** / Kanzawa, Hiroaki; Oyamatsu, Kazuhiro; Sumiyoshi, Kohsuke; Takano, Masatoshi.

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

*Proceedings of Science.*10th Symposium on Nuclei in the Cosmos, NIC 2008, Mackinac Island, MI, United States, 08/7/27.

}

TY - GEN

T1 - Nuclear many-body approach for supernova EOS

T2 - Thomas-fermi calculations of non-uniform nuclear matter

AU - Kanzawa, Hiroaki

AU - Oyamatsu, Kazuhiro

AU - Sumiyoshi, Kohsuke

AU - Takano, Masatoshi

PY - 2008

Y1 - 2008

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 AV18 two-body potential and the UIX three-body potential. The maximum mass of the cold neutron star with this EOS is 2.2 M ⊙. Making use of uncertainty of the three-body nuclear force, adjustable parameters in the EOS are tuned so that the Thomas-Fermi calculations for β-stable nuclei reproduce the empirical data. The obtained EOS is appropriate for constructing a new nuclear EOS table for supernova simulations.

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 AV18 two-body potential and the UIX three-body potential. The maximum mass of the cold neutron star with this EOS is 2.2 M ⊙. Making use of uncertainty of the three-body nuclear force, adjustable parameters in the EOS are tuned so that the Thomas-Fermi calculations for β-stable nuclei reproduce the empirical data. The obtained EOS is appropriate for constructing a new nuclear EOS table for supernova simulations.

UR - http://www.scopus.com/inward/record.url?scp=84887290669&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84887290669&partnerID=8YFLogxK

M3 - Conference contribution

AN - SCOPUS:84887290669

BT - Proceedings of Science

ER -