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

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 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

Role of relativistic effects and three-body forces in nuclear matter properties

2019 ◽  
Vol 99 (2) ◽  
Author(s):  
S. Heidari ◽  
S. Zaryouni ◽  
H. R. Moshfegh ◽  
S. Goudarzi
Keyword(s):  
Nuclear Matter ◽  
Relativistic Effects ◽  
Body Forces ◽  
Three Body

Three-Body Forces in Nuclear Matter.

1968 ◽  
Vol 21 (14) ◽  
pp. 1030-1030 ◽  
Author(s):  
Bruce H. J. McKellar ◽  
R. Rajaraman
Keyword(s):  
Nuclear Matter ◽  
Body Forces ◽  
Three Body

TOWARD A NEW PARAMETERIZATION OF THE GOGNY FORCE: NEUTRON MATTER AND NUCLEAR BINDING ENERGIES

2006 ◽  
Vol 15 (02) ◽  
pp. 339-345 ◽  
Author(s):  
F. CHAPPERT ◽  
M. GIROD
Keyword(s):  
Equation Of State ◽  
Nuclear Matter ◽  
Variational Calculation ◽  
Binding Energies ◽  
Neutron Matter ◽  
Saturation Point ◽  
Nuclear Binding

A new parameterization of the effective Gogny interaction is investigated. It has the property of fitting the neutron matter Equation Of State (EOS) as predicted by a variational calculation. Its properties in nuclear matter (saturation point, compressibility, …) and in nuclei (binding energies) are presented.

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.

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