Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter
- Received Date: 2003-02-26
- Accepted Date: 1900-01-01
- Available Online: 2003-12-05
Abstract: The proton and neutron 1S0 pairing gaps in β-stable neutron star matter have been studied by using the isospin dependent Brueckner-Hartree-Fock approach and the BCS theory. We have concentrated on investigating and discussing the effect of three-body force. The calculated results indicate that the three-body force has only a small effect on the neutron 1S0 superfluidity in β-stable neutron matter, i.e., it leads to a small reduction of the neutron 1S 0 paring gap. However the three-body force not only suppresses strongly the strength of the proton1S0 superfluidity in β-stable neutron star matter but also reduces largely the density domain for the proton 1S0 superfluidity phase from ρ B<0.45fm－3 to ρB<0.3fm－3. It is also shown that the three-body force enhances largely the proton fraction in β-stable neutron star matter at high densities.