PAIRING INTERACTION POTENTIAL WITH REALISTIC FORCE IN NEUTRON AND NUCLEAR MATTER

2006 ◽  
Vol 15 (08) ◽  
pp. 1769-1777
Author(s):  
CAIWAN SHEN
Keyword(s):  
Nuclear Matter ◽  
Interaction Potential ◽  
Effective Interaction ◽  
Nucleon Nucleon ◽  
Pairing Interaction ◽  
Nucleon Interaction ◽  
Explicit Formulas ◽  
Nucleon Nucleon Interaction ◽  
Realistic Force

Using the realistic nucleon-nucleon interaction, we studied the pairing interaction potential for 1S0 and 3S1 channel in neutron and nuclear matter. The explicit formulas are given for the calculation. It is found that the screening using realistic force is much smaller than that using effective interaction, for instance, Gogny force or G-matrix.

The L-G Phase Transition and the Nucleon–Nucleon Interaction Potential within QHD-I Model

2003 ◽  
Vol 18 (29) ◽  
pp. 2029-2037
Author(s):  
Jin Meng ◽  
Jiarong Li ◽  
Jisheng Chen
Keyword(s):  
Phase Transition ◽  
Nuclear Matter ◽  
Interaction Potential ◽  
Yukawa Potential ◽  
Nucleon Nucleon ◽  
Nucleon Interaction ◽  
Nucleon System ◽  
Debye Mass ◽  
Dense Nuclear Matter ◽  
Nucleon Nucleon Interaction

The nucleon–nucleon interaction potential in hot/dense nuclear matter is studied within the QHD-I model. We find that a Yukawa potential, which contains attractive and repulsive terms, acting between nucleons is modified by the variation of the Debye mass. In particular, a nucleon system described by this Yukawa potential will be unbound at some critical T and μ. The critical point is very close to that of the L-G phase transition given in the literatures.

PROTON SUPERFLUIDITY IN NEUTRON STAR MATTER WITH AN EFFECTIVE INTERACTION

1995 ◽  
Vol 04 (04) ◽  
pp. 843-848 ◽  
Author(s):  
G. LAZZARI ◽  
F.V. DE BLASIO
Keyword(s):  
Neutron Star ◽  
Proton Energy ◽  
Energy Gap ◽  
Effective Interaction ◽  
Nucleon Nucleon ◽  
Neutron Star Matter ◽  
Nucleon Interaction ◽  
Effective Force ◽  
Nucleon Nucleon Interaction ◽  
Considerable Range

The isotropic proton superfluidity in Neutron Star Matter is evaluated in the conventional BCS approach using Gogny effective force as the nucleon-nucleon interaction. We have found that, neglecting the polarizability effects and including different proton concentrations in neutron star matter, the 1S0 proton energy gap is considerably smaller than the corresponding neutron isotropic gap. It is shown that at higher densities proton superfluidity could prevail in a considerable range of density in the interior of a neutron star.

Nucleon-nucleon interaction in nuclear matter

1977 ◽  
Vol 16 (2) ◽  
pp. 777-783 ◽  
Author(s):  
Sadhan K. Adhikari ◽  
H. T. Coelho ◽  
F. A. Bezerra Coutinho ◽  
Y. Nogami
Keyword(s):  
Nuclear Matter ◽  
Nucleon Nucleon ◽  
Nucleon Interaction ◽  
Nucleon Nucleon Interaction
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