The relativistic neutrino emissivity of the nucleonic direct URCA processes in neutron star matter is investigated within the relativistic Hartree-Fock approximation. We particularly study the influences of the tensor...The relativistic neutrino emissivity of the nucleonic direct URCA processes in neutron star matter is investigated within the relativistic Hartree-Fock approximation. We particularly study the influences of the tensor couplings of vector mesons ω and ρ on the nucleonic direct URCA processes. It is found that the inclusion of the tensor couplings of vector mesons w and p can slightly increase the maximum mass of neutron stars. In addition, the results indicate that the tensor couplings of vector mesons ω and ρ lead to obvious enhancement of the total neutrino emissivity for the nucleonic direct URCA processes, which must accelerate the cooling rate of the non- superfluid neutron star matter. However, when considering only the tensor coupling of vector meson ρ, the neutrino emissivity for the nucleonic direct URCA processes slightly declines at low densities and significantly increases at high densities. That is, the tensor coupling of vector meson ρ leads to the slow cooling rate of a low-mass neutron star and rapid cooling rate of a massive neutron star.展开更多
In the framework of the relativistic mean field theory,it is found that recently discovered PSR J1614-2230 with mass of 1.97±0.04Mʘmay include hyperons when the weakly interacting light boson(WILB)is considered.T...In the framework of the relativistic mean field theory,it is found that recently discovered PSR J1614-2230 with mass of 1.97±0.04Mʘmay include hyperons when the weakly interacting light boson(WILB)is considered.To describe PSR J1614−2230 with the equation of state(EOS)including hyperons,the characteristic scale of the WILB(g^(2)/μ^(2))should lie in the range of 13–46(24–46)GeV^(−2) with the weak(strong)hyperon-hyperon(YY)interaction.The measurements of inertial momentum and the total neutrino luminosity of the neutron star could be used to further constrain the characteristic scale of the WILB.Before more stringent constraint on the WILB is given,the mass measurement of the neutron star could not exclude any soft EOS.展开更多
基金Supported by the National Natural Science Foundation of China under Grant Nos 11447165,11373047 and 11265009the Youth Innovation Promotion Association of Chinese Academy of Sciences under Grant No 2016056
文摘The relativistic neutrino emissivity of the nucleonic direct URCA processes in neutron star matter is investigated within the relativistic Hartree-Fock approximation. We particularly study the influences of the tensor couplings of vector mesons ω and ρ on the nucleonic direct URCA processes. It is found that the inclusion of the tensor couplings of vector mesons w and p can slightly increase the maximum mass of neutron stars. In addition, the results indicate that the tensor couplings of vector mesons ω and ρ lead to obvious enhancement of the total neutrino emissivity for the nucleonic direct URCA processes, which must accelerate the cooling rate of the non- superfluid neutron star matter. However, when considering only the tensor coupling of vector meson ρ, the neutrino emissivity for the nucleonic direct URCA processes slightly declines at low densities and significantly increases at high densities. That is, the tensor coupling of vector meson ρ leads to the slow cooling rate of a low-mass neutron star and rapid cooling rate of a massive neutron star.
文摘In the framework of the relativistic mean field theory,it is found that recently discovered PSR J1614-2230 with mass of 1.97±0.04Mʘmay include hyperons when the weakly interacting light boson(WILB)is considered.To describe PSR J1614−2230 with the equation of state(EOS)including hyperons,the characteristic scale of the WILB(g^(2)/μ^(2))should lie in the range of 13–46(24–46)GeV^(−2) with the weak(strong)hyperon-hyperon(YY)interaction.The measurements of inertial momentum and the total neutrino luminosity of the neutron star could be used to further constrain the characteristic scale of the WILB.Before more stringent constraint on the WILB is given,the mass measurement of the neutron star could not exclude any soft EOS.
