¹S₀ Nucleon Superfluidity in Neutron Star Matter

【摘要】 We investigate the nucleon superfluidity in the ¹S₀ channel in neutron star matter using the relativistic mean field theory and the BCS theory.We discuss particularly the influence of the isovector scalar interaction which is considered by exchanging 5 meson on the nucleon superfluidity.It is found that the 5 meson leads to a growth of the nucleon ¹S₀ pairing energy gaps in a middle density range of the existing nucleon superHuidity.In addition,when the density PB > 0.36 fm^-3,the proton 1S₀ pairing- energy gap obviously decreases.The density range of the proton 1^S₀ superfluidity is narrowed due to the presence of d mesons.In our results,the 5 meson not only changes the EOS and bulk properties but also changes the cooling properties of neutron stars.更多还原

【Abstract】 We investigate the nucleon superfluidity in the ¹S₀ channel in neutron star matter using the relativistic mean field theory and the BCS theory.We discuss particularly the influence of the isovector scalar interaction which is considered by exchanging 5 meson on the nucleon superfluidity.It is found that the 5 meson leads to a growth of the nucleon ¹S₀ pairing energy gaps in a middle density range of the existing nucleon superHuidity.In addition,when the density PB > 0.36 fm^-3,the proton 1S₀ pairing- energy gap obviously decreases.The density range of the proton 1^S₀ superfluidity is narrowed due to the presence of d mesons.In our results,the 5 meson not only changes the EOS and bulk properties but also changes the cooling properties of neutron stars.更多还原