1S0 Nucleon Superfluidity in Neutron Star Matter
2013
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 δ meson on the nucleon superfluidity. It is found that the δ meson leads to a growth of the nucleon 1S0 pairing energy gaps in a middle density range of the existing nucleon superfluidity. In addition, when the density ρB > 0.36 fm−3, the proton 1S0 pairing energy gap obviously decreases. The density range of the proton 1S0 superfluidity is narrowed due to the presence of δ mesons. In our results, the δ meson not only changes the EOS and bulk properties but also changes the cooling properties of neutron stars.
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