Published May 12, 2010 | Version v1
Journal article Metadata-only

Nucleon Superfluidity in Asymmetric Nuclear Matter and Neutron Star Matter

Creators

  • 1. Institute of Modern Physics, Chinese Academy of Science, Lanzhou 730000 (China)
  • 2. Department of Physics and Astrophysics, Catania University, Via Santa Sofia 64, I-95123 (Italy)

Description

We have investigate the nucleon superfluidity in asymmetric nuclear matter and neutron star matter by using the Brueckner-Hartree-Fock approach and the BCS theory. We have predicted the isospin-asymmetry dependence of the nucleon superfluidity in asymmetric nuclear matter and discussed particularly the effect of microscopic three-body forces. It has been shown that the three-body force leads to a strong suppression of the proton 1S0 superfluidity in β-stable neutron star matter. Whereas the microscopic three-body force is found to enhance remarkably the 3PF2 neutron superfluidity in neutron star matter and neutron stars.

Additional details

Identifiers

DOI
10.1063/1.3442600;

Publishing Information

Journal Title
AIP Conference Proceedings
Journal Volume
1235
Journal Issue
1
Journal Page Range
p. 235-241
ISSN
0094-243X
CODEN
APCPCS

Conference

Title
7. Japan-China joint nuclear physics symposium
Dates
9-13 Nov 2009
Place
Tsukuba (Japan)

INIS

Country of Publication
United States
Country of Input or Organization
International Atomic Energy Agency (IAEA)
INIS RN
41096571
Subject category
S73: NUCLEAR PHYSICS AND RADIATION PHYSICS;
Resource subtype / Literary indicator
Conference
Descriptors DEI
ASYMMETRY; BCS THEORY; HARTREE-FOCK METHOD; ISOSPIN; NEUTRON SOURCES; NEUTRON STARS; NEUTRONS; NUCLEAR MATTER; NUCLEON-NUCLEON INTERACTIONS; PROTONS; SUPERFLUIDITY; THREE-BODY PROBLEM
Descriptors DEC
APPROXIMATIONS; BARYON-BARYON INTERACTIONS; BARYONS; CALCULATION METHODS; ELEMENTARY PARTICLES; FERMIONS; HADRON-HADRON INTERACTIONS; HADRONS; INTERACTIONS; MANY-BODY PROBLEM; MATTER; NUCLEONS; PARTICLE INTERACTIONS; PARTICLE PROPERTIES; PARTICLE SOURCES; RADIATION SOURCES; STARS

Optional Information

Notes
(c) 2010 American Institute of Physics