Direct Urca Processes Involving Proton 1S0 Superfluidity in Neutron Star Cooling

• 来源期刊: 理论物理通讯（英文版）
• 年，卷（期）: 2018,（4）
• 页码范围: 425-433
• 页数: 9页
• 语种: 英文
• DOI: 10.1088/0253-6102/69/4/425

摘要

A detailed description of the baryon direct Urca processes A:n → p + e + (v)e,B:A → p + e + (v)e and C:(I)-→ A + e + (v)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 1S0 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 1S0 superfluid due to the higher threshold density of the reaction C,which will further speed up the two pulsars cooling.