Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter

  • 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.
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LI Zeng-Hua, LU Guang-Cheng and ZUO Wei. Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter[J]. Chinese Physics C, 2003, 27(12): 1084-1088.
LI Zeng-Hua, LU Guang-Cheng and ZUO Wei. Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter[J]. Chinese Physics C, 2003, 27(12): 1084-1088. shu
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Received: 2003-02-26
Revised: 1900-01-01
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Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter

    Corresponding author: ZUO Wei,
  • Institute of Modern Physics,CAS,Lanzhou 730000,China

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.

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