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1S0 Nucleon Superfluidity in Neutron Star Matter |
| XU Yan1**, LIU Guang-Zhou2, LIU Cheng-Zhi1, FAN Cun-Bo1, HAN Xing-Wei1, ZHU Ming-Feng2, WANG Hong-Yan3, ZHANG Xiao-Jun1 |
1Changchun Observatory, National Astronomical Observatories, Chinese Academy of Sciences, Changchun 130117
2Center for Theoretical Physics, Jilin University, Changchun 130012
3College of Physics, Beihua University, Jilin 132013
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XU Yan, LIU Guang-Zhou, LIU Cheng-Zhi et al 2013 Chin. Phys. Lett. 30 062101 |
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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 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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Received: 01 April 2013
Published: 31 May 2013
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