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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2003, Vol. 27> Issue(12) : 1084-1088 

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

  •  Institute of Modern Physics,CAS,Lanzhou 730000,China

  • 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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    [1] . Migdal A B et al.Sov.Phys.JETP ,1960,10:1762. Pethick C J et al.Annu.Rev.Nucl.Part.Sci.,1995,45:4293. Pines D ,Alpar M A .Nature,1985,316:274. Shapiro S L ,Teukolsky S A .Black Holes,White Dwrfs and Neutron Stars,New York:John Wiley,19835. Baldo M ,Cugnon J ,Lejeune A et al.Nucl.Phys.,1992,A536:3496. Elgaroy O et al.Phys.Rev.Lett.,1996,77:14287. ZUO Wei et al.High Energy Phys.and Nucl.Phys.,2002,26:1134(in Chinese)(左维等.高能物理与核物理,2002,26:1134)8. Migdal A B .Theory of Finite Fermi Systems and Applications to Atomic Nuclei,London:Interscience Publisher,19679. Ring P ,Schuck P .The Nuclear Many-body Problem,New York:Springer-Verlag,198010. Baldo M ,Cugnon J,Lejeune A et al.Nucl.Phys.,1990,A515:40911. Lombardo U ,Schulze H J .Lecture Notes in Physics,2001,578:3012. Clark J W ,Kallman C G ,Yang C H et al.Phys.Lett.,1976,B61:33113. Ainsworth T L ,Wambach J ,Pines D .Phys.Lett.,1989,B222:17314. Schulze H J,Cugnon J ,Lejeune A et al.Phys.Lett.,1996,B375:115. Day B D .Rev.Mod.Phys.,1967,39:719;Jeukenne J P et al.Phys.Rep.,1976,25:83;ZUO Wei et al.High Energy Phys.and Nucl.Phys.,2002,26:703(in Chinese)(左维等.高能物理与核物理,2002,26:703) 16. Wiringa R B ,Stoks V G J,Schiavilla R .Phys.Rev.,1995,C51:2817. Grange P et al.Phys.Rev.,1989,C40:1040 18. SONG H Q et al.Phys.Rev.Lett.,1998,81:158419. Lattimer J M ,Pethick C J,Prakash M et al.Phys.Rev.Lett.,1991,66:2701;Pethick C J.Rev.Mod.Phys.,1992,64:113320. ZUO Wei et al.HEPNP ,2002,26:1238(in Chinese)(左维等.高能物理与核物理,2002,26:1238)21. Machleidt R .Adv.Nucl.Phys.,1989,16:18922. ZUO Wei et al.Phys.Rev.,2002,C66:03730323. Bombaci I ,Lombardo U .Phys.Rev.,1991,C44:1892

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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
  • 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.

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