超子中子星性质的温度效应

Effect of Temperature on Hyperon Neutron Star

从相对论平均场理论出发 ,考虑核子、超子和介子的相互作用 ,研究了温度对中子星组成粒子、状态方程和中子星质量等的影响 .发现温度越高 ,超子在中子星内部出现时的重子数密度越低 .当密度较高时 ,中子星的核心区主要由超子组成 ,即中子星转变成以奇异粒子为主要成分的超子星 ,并且这种转变受到温度的影响 ,温度越高 ,转变密度越低 .由于超子的出现 ,中子星核心高密度区域的状态方程 ,对于不同温度 ,差别不大 ,所以有限温度中子星的最大质量都在 1 8M⊙ 附近 .

The influences of temperature on the constitutes, equations of state and masses of neutron star are studied in the frame work of the relativistic mean field theory for an interacting nucleons, hyperons, and mesons system. It is found that the appearing density of hyperons becomes smaller with temperature increasing. At higher hadron densities, the core of the neutron star is dominated by hyperons, in another words a neutron star transits into a hyperon star. The effects of temperature on the transition of a neutron star to a hyperon star are also investigated. The higher the temperature is, the smaller the transition density is. And it is also found that the equations of state for hadronic matter in the core region of a neutron star are approximately the same at different temperature. The calculated maximum masses of neutron stars are about 1 8 M ⊙, which are in consistence with the observation.