Direct Urca Processes Involving Proton ^1S0 Superfluidity in Neutron Star Cooling
Direct Urca Processes Involving Proton ~1S_0 Superfluidity in Neutron Star Cooling作者机构：Changchun Observatory National Astronomical Observatories CAS Changchun 130117 China College of Science Nanjing Forestry University Nanjing 210037 China Center for Theoretical Physics Jilin University Changchun 130023 China Institute of Theoretical Physics Chinese Academy of Sciences Beijing 100190 China
出 版 物：《Communications in Theoretical Physics》 (理论物理通讯（英文版）)
年 卷 期：2018年第69卷第4期
页 面：425-433页
核心收录：
学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学]
基 金：Supported by the National Natural Science Foundation of China under Grant Nos.11447165,11373047,11404336 and U1731240 Youth Innovation Promotion Association,CAS under Grant No.2016056 the Development Project of Science and Technology of Jilin Province under Grant No.20180520077JH
主 题：neutron star the proton ^1S0 superfluid
摘 要：A detailed description of the baryon direct Urca processes A: n → p + e + ν_e, B: Λ→ p + e + ν_e and C: Ξ^-→Λ + e + ν_e related to the neutron star cooling is given in the relativistic mean field approximation. The contributions of the reactions B and C on the neutrino luminosity are calculated by means of the relativistic expressions of the neutrino energy losses. Our results show that the total neutrino luminosities of the reactions A, B and C within the mass range(1.603–2.067) M_⊙((1.515–1.840) M_⊙ for TM1 model) for GM1 model are larger than the corresponding values for neutron star without hyperons. Furthermore, although the neutrino emissivity of the reaction A is suppressed with the appearance of the proton ~1S_0 superfluid, the contribution of the reactions B and C can still quicken a massive neutron star cooling. In particular, the reaction C in PSR J1614-2230 and J0348+0432 is not suppressed by the proton ~1S_0 superfluid due to the higher threshold density of the reaction C, which will further speed up the two pulsars cooling.
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