大质量中子星可包含超子

在相对论平均场理论(RMFT)框架下考虑超子自由度, 用7个参数组计算中子星的质量, 并分析超子耦合常数对中子星最大质量的影响. 结果表明: 对应状态方程（EOS）较硬的3个参数组（NLSH,NL3,NL2）, 中子星的最大质量可达已观测到中子星PSR J0348+0432和PSR J1614-2230及双中子星合并GW170817中给出的质量, 即大质量中子星结构中可包含超子相； 随着超子耦合常数χ的增大, 状态方程变硬, 中子星最大质量增大； 当NLSH参数组的χ≥0.6时, 中子星最大质量均大于2M⊙（M⊙为太阳质量）. 因此, 合理选择状态方程较硬的参数组与较强超子耦合常数可获得大质量中子星.

Massive Neutron Star Can Contain Hyperon

We calculated the mass of the neutron star by using seven parameter sets and considering the hyperon degrees of freedom in the framework of the relativistic mean field theory (RMFT), and analyzed the influence of coupling constants of hyperons on the maximum mass of neutron star. The results show that adopting three type sets （NLSH,NL3,NL2）in accordance with relative stiff equation of state (EOS), the maximum mass of neutron star can reach the mass given in the observed massive neutron star PSR J0348+0432,PSR J1614 2230 and the binary neutron star merger GW170817, the massive neutron star can contain hyperon phase. With the increase of the hyperon coupling constant (χ), the equation of state stiffens, and the maximum mass of neutron star increases. When χ≥0.6 of the NLSH parameter set, the maximum mass of neutron star is more than 2M⊙（M⊙ is mass of the sun）. Therefore, the massive neutron star can be obtained by choosing relative stiff EOS from three parameter sets and relative strong coupling constants of hyperons.