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 |
|---|---|
| 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 |
|---|---|
| Country | United States |
| City | Mackinac Island, MI |
| Period | 08/7/27 → 08/8/1 |
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ASJC Scopus subject areas
- General
Cite this
Nuclear many-body approach for supernova EOS : Thomas-fermi calculations of non-uniform nuclear matter. / Kanzawa, Hiroaki; Oyamatsu, Kazuhiro; Sumiyoshi, Kohsuke; Takano, Masatoshi.
Proceedings of Science. 2008.Research output: Chapter in Book/Report/Conference proceeding › Conference contribution
}
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
BT - Proceedings of Science
ER -