scholarly journals Nuclear three-body force effect on a kaon condensate in neutron star matter

2004 ◽  
Vol 70 (5) ◽  
Author(s):  
W. Zuo ◽  
A. Li ◽  
Z. H. Li ◽  
U. Lombardo
Keyword(s):  
Neutron Star ◽  
Body Force ◽  
Neutron Star Matter ◽  
Force Effect ◽  
Kaon Condensate ◽  
Three Body

scholarly journals Constraints on Microscopic and Phenomenological Equations of State of Dense Matter from GW170817

Universe ◽  
2019 ◽  
Vol 5 (10) ◽  
pp. 204 ◽  
Author(s):  
Domenico Logoteta ◽  
Ignazio Bombaci
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Equations Of State ◽  
Mean Field ◽  
Dense Matter ◽  
Neutron Star Matter ◽  
Field Approach ◽  
Relativistic Mean Field ◽  
Three Body ◽  
Good Agreement

We discuss the constraints on the equation of state (EOS) of neutron star matter obtained by the data analysis of the neutron star-neutron star merger in the event GW170807. To this scope, we consider two recent microscopic EOS models computed starting from two-body and three-body nuclear interactions derived using chiral perturbation theory. For comparison, we also use three representative phenomenological EOS models derived within the relativistic mean field approach. For each model, we determine the β -stable EOS and then the corresponding neutron star structure by solving the equations of hydrostatic equilibrium in general relativity. In addition, we calculate the tidal deformability parameters for the two neutron stars and discuss the results of our calculations in connection with the constraints obtained from the gravitational wave signal in GW170817. We find that the tidal deformabilities and radii for the binary’s component neutron stars in GW170817, calculated using a recent microscopic EOS model proposed by the present authors, are in very good agreement with those derived by gravitational waves data.

Three-body-force effect on nucleus-nucleus elastic scattering

2009 ◽  
Vol 79 (1) ◽  
Author(s):  
T. Furumoto ◽  
Y. Sakuragi ◽  
Y. Yamamoto
Keyword(s):  
Elastic Scattering ◽  
Body Force ◽  
Force Effect ◽  
Three Body

Proton-4He elastic scattering at 350–1728MeV energies: Three-body force effect

2018 ◽  
Vol 27 (03) ◽  
pp. 1850020
Author(s):  
M. A. Hassan ◽  
H. E. A. Awd-Allah ◽  
T. N. E. Salama ◽  
Z. S. Hassan
Keyword(s):  
Elastic Scattering ◽  
Multiple Scattering ◽  
Scattering Theory ◽  
Body Force ◽  
Nucleon Force ◽  
Force Effect ◽  
Optical Limit ◽  
Optical Limit Approximation ◽  
Three Body ◽  
Limit Approximation

An approach for the three-body force effect is used to study p-[Formula: see text] elastic scattering at energies 350–1728[Formula: see text]MeV. The multiple scattering theory of Glauber and the optical limit approximation are used in calculations of elastic scattering differential cross-section at 350, 600, 800, 1000 and 1728[Formula: see text]MeV. The inclusion of 2[Formula: see text]-exchange three-nucleon force improves the agreement with the experimental data for both approximations. The results of optical limit approximation without three-nucleon force effect are clearly smaller than the results of multiple scattering theory for [Formula: see text] due to the absence of multiple scattering terms in the first. However, with inclusion of three-nucleon force, the results of both approximations are approximately similar.

CONSISTENT THREE-BODY FORCE WITH BONN B POTENTIAL AND NEUTRON STAR STRUCTURE

2010 ◽  
Vol 19 (08n09) ◽  
pp. 1727-1733 ◽  
Author(s):  
Z. H. LI ◽  
U. LOMBARDO ◽  
H.-J. SCHULZE ◽  
W. ZUO
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Symmetry Energy ◽  
Body Force ◽  
Nucleon Force ◽  
Nucleon Potential ◽  
Saturation Properties ◽  
Nuclear Equation Of State ◽  
Neutron Star Mass ◽  
Three Body

Microscopic three-nucleon force consistent with the Bonn B two-nucleon potential is constructed, which includes Δ(1232), Roper, and nucleon-antinucleon excitation contributions. Recent results for the choice of the meson parameters are discussed. The forces are used in Brueckner calculations and the saturation properties of nuclear matter are determined. At the high densities, the nuclear equation of state and the symmetry energy are calculated. The corresponding neutron star mass-radius relations are presented.

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