This paper investigates the third series of the 2s+1 p0 helium states. The anisotropism of the electronic distribution is presented, the partial-wave compositions of the states are compared with each other, and the an...This paper investigates the third series of the 2s+1 p0 helium states. The anisotropism of the electronic distribution is presented, the partial-wave compositions of the states are compared with each other, and the angular correlation is intuitively shown by the shape-density. Two types of radial-radial correlation, namely, the "gradually push" and the "sudden transition", have been identified and the approximate symmetry with respect to the interchange of r1 and r2 has been evaluated.展开更多
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 approximatio...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.展开更多
文摘This paper investigates the third series of the 2s+1 p0 helium states. The anisotropism of the electronic distribution is presented, the partial-wave compositions of the states are compared with each other, and the angular correlation is intuitively shown by the shape-density. Two types of radial-radial correlation, namely, the "gradually push" and the "sudden transition", have been identified and the approximate symmetry with respect to the interchange of r1 and r2 has been evaluated.
基金Supported by the National Natural Science Foundation of China under Grant Nos.11447165,11373047,11404336 and U1731240Youth Innovation Promotion Association,CAS under Grant No.2016056the Development Project of Science and Technology of Jilin Province under Grant No.20180520077JH
文摘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.
