许妍, 喻孜, 张晓军, 范存波, 刘广洲, 赵恩广, 黄修林, 刘承志
理论物理通讯. 2018, 69(04): 425-433.
A detailed description of the baryon direct Urca processes A:n→p+e+νe,B:Λ→p+e+νe and C:Ξ-→Λ+e+νe 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.