scholarly journals Nuclear-matter equation of state with consistent two- and three-body perturbative chiral interactions

2014 ◽  
Vol 89 (4) ◽  
Author(s):  
L. Coraggio ◽  
J. W. Holt ◽  
N. Itaco ◽  
R. Machleidt ◽  
L. E. Marcucci ◽  
...  
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Chiral Interactions ◽  
Three Body

scholarly journals Hot nuclear matter equation of state with a three-body force

2004 ◽  
Vol 69 (6) ◽  
Author(s):  
W. Zuo ◽  
Z. H. Li ◽  
A. Li ◽  
G. C. Lu
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Body Force ◽  
Three Body

scholarly journals Equation of state of dense nuclear matter and neutron star structure from nuclear chiral interactions

2018 ◽  
Vol 609 ◽  
pp. A128 ◽  
Author(s):  
Ignazio Bombaci ◽  
Domenico Logoteta
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Symmetric Nuclear Matter ◽  
Heavy Nuclei ◽  
Hartree Fock ◽  
Binary Neutron Star ◽  
Dense Nuclear Matter ◽  
Three Body

Aims. We report a new microscopic equation of state (EOS) of dense symmetric nuclear matter, pure neutron matter, and asymmetric and β-stable nuclear matter at zero temperature using recent realistic two-body and three-body nuclear interactions derived in the framework of chiral perturbation theory (ChPT) and including the Δ(1232) isobar intermediate state. This EOS is provided in tabular form and in parametrized form ready for use in numerical general relativity simulations of binary neutron star merging. Here we use our new EOS for β-stable nuclear matter to compute various structural properties of non-rotating neutron stars. Methods. The EOS is derived using the Brueckner–Bethe–Goldstone quantum many-body theory in the Brueckner–Hartree–Fock approximation. Neutron star properties are next computed solving numerically the Tolman–Oppenheimer–Volkov structure equations. Results. Our EOS models are able to reproduce the empirical saturation point of symmetric nuclear matter, the symmetry energy Esym, and its slope parameter L at the empirical saturation density n0. In addition, our EOS models are compatible with experimental data from collisions between heavy nuclei at energies ranging from a few tens of MeV up to several hundreds of MeV per nucleon. These experiments provide a selective test for constraining the nuclear EOS up to ~4n0. Our EOS models are consistent with present measured neutron star masses and particularly with the mass M = 2.01 ± 0.04 M⊙ of the neutron stars in PSR J0348+0432.

Equation of State of Nuclear Matter and the Nuclear Three-Body Force

2008 ◽  
Author(s):  
H. Kanzawa ◽  
K. Oyamatsu ◽  
K. Sumiyoshi ◽  
M. Takano ◽  
Hideyuki Sakai ◽  
...  
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Body Force ◽  
Three Body

EQUATION OF STATE AND SINGLE-PARTICLE PROPERTIES OF NEUTRON-RICH NUCLEAR MATTER

2008 ◽  
Vol 17 (supp01) ◽  
pp. 256-271
Author(s):  
WEI ZUO
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Single Particle ◽  
Body Force ◽  
Research Work ◽  
Momentum Dependence ◽  
Particle Properties ◽  
Saturation Properties ◽  
Nucleon Superfluidity ◽  
Three Body

We report our research work on the equation of state (EOS) and single-particle (s.p.) properties of neutron-rich nuclear matter within the framework of the Brueckner–Bethe–Goldstone approach extended to include a microscopic three-body force (TBF). We show that inclusion of the TBF provide a largely improvement of the predicted nuclear matter saturation properties and leads to a strongly stiffening of the density dependence of symmetry energy at high densities. The neutron effective mass turns out to be greater than the proton one in neutron-rich nuclear matter in both cases of including and not including the TBF. The TBF induces a strongly repulsive rearrangement contribution to nucleon s.p. potential at high densities and large momenta. The TBF rearrangement contribution reduces considerably the attraction of the neutron and proton s.p. potentials and enhances strongly their momentum-dependence at high densities and high momenta. The TBF effect on nucleon superfluidity in neutron star matter has also been discussed.

Neutron star properties from optimised chiral nuclear interactions

2018 ◽  
Vol 35 ◽  
Author(s):  
D. Logoteta ◽  
I. Bombaci
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Nuclear Interaction ◽  
Binding Energies ◽  
Leading Order ◽  
Nuclear Forces ◽  
Hartree Fock ◽  
First Case ◽  
Three Body

AbstractWe adopt two- and three-body nuclear forces derived at the next-to-next-to-leading-order in the framework of effective chiral perturbation theory to calculate the equation of state of β-stable neutron star matter using the Brueckner–Hartree–Fock many-body approach. We use the recent optimized chiral two-body nuclear interaction at next-to-next-to-leading-order derived by Ekström et al. and two different parametrizations of the three-body next-to-next-to-leading-order interaction: the first one is fixed to reproduce the saturation point of symmetric nuclear matter while the second one is fixed to reproduce the binding energies of light atomic nuclei. We show that in the second case the properties of nuclear matter are not well determined whereas in the first case various empirical nuclear matter properties around the saturation density are well reproduced. We finally calculate various neutron star properties and in particular the mass-radius and mass-central density relations. We find that the adopted interactions based on a fully microscopic framework, are able to provide an equation of state which is consistent with the present data of measured neutron star masses.

THREE NUCLEON CORRELATIONS IN NUCLEAR MEDIUM

2003 ◽  
Vol 18 (02n06) ◽  
pp. 317-321
Author(s):  
H. Q. SONG ◽  
M. BALDO ◽  
A. FIASCONARO ◽  
G. GIANSIRACUSA ◽  
U. LOMBARDO
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Nuclear Medium ◽  
Main Term ◽  
Saturation Point ◽  
Good Convergence ◽  
Body Forces ◽  
Three Body ◽  
Line Level

The equation of state(EOS) of nuclear matter is studied up to the three-hole-line level of approximation in the Behte-Brueckner-Goldstone expansion. The results indicate a good convergence of the theory. The fact that the resulting EOS does not reproduce the empirical saturation point suggests that the three-body forces are most likely the main term missing in the nuclear Hamiltonian.

Nuclear matter equation of state and three-body forces

2012 ◽  
Vol 75 (4) ◽  
pp. 430-438 ◽  
Author(s):  
H. M. M. Mansour ◽  
A. M. A. Algamoudi
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Body Forces ◽  
Three Body

EQUATION OF STATE OF ASYMMETRIC NUCLEAR MATTER WITH GOGNY AND COULOMB INTERACTIONS

1990 ◽  
Vol 05 (14) ◽  
pp. 1071-1080 ◽  
Author(s):  
S. W. HUANG ◽  
M. Z. FU ◽  
S. S. WU ◽  
S. D. YANG
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Coulomb Interaction ◽  
Chemical Potential ◽  
Compression Modulus ◽  
Nucleon Nucleon ◽  
Effective Density ◽  
Coulomb Interactions ◽  
Asymmetric Nuclear Matter ◽  
Nucleon Nucleon Interaction

The equation of state of the asymmetric nuclear matter is calculated with the Gogny D1 effective density-dependent nucleon-nucleon interaction and the Coulomb interaction in the framework of the finite-temperature HF method with the rearrangement term. The dependence of the thermodynamical properties such as the critical temperature of the liquid-gas phase transition, the chemical potential, the compression modulus and the entropy on the Coulomb interaction in nuclear matter is treated by using a shielded two-body Coulomb potential and this method has been found to be a reasonable and effective approach.

scholarly journals Constraining the equation of state of dense nuclear matter using thermal emission of neutron stars

2020 ◽  
Vol 1667 ◽  
pp. 012001
Author(s):  
Nicolas Baillot d’Étivaux ◽  
Jérôme Margueron ◽  
Sebastien Guillot ◽  
Natalie Webb ◽  
Màrcio Catelan ◽  
...  
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Thermal Emission ◽  
Dense Nuclear Matter
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