能通过大质量中子星转动惯量来限定超子参数吗?

在相对论平均场理论（RMFT）框架内，使用GL91参数组结合超核数据和大质量中子星的观测数据限定超子标量耦合参数X_σ=0.59~1.0，用慢转近似计算了大质量中子星和前中子星的转动惯量。当X_σ从0.59增加到1.0，中子星（前中子星）的最大转动惯量增幅达89%（60%）。在同样的变化范围内，用Crab的观测数据，计算得到中子星（前中子星）的最大能量损失（dE/dt）的增幅为44%（25%），最大磁场增幅为48%（38%）。相比于前中子星，中子星的性质对超子参数更为敏感。当X_σ从0.59增加到1.0，PSR J0348+0432的转动惯量和dE/dt的增幅均为14%，而磁场减幅为10%。如果天文观测能够给出中子星转动惯量的上限，或者同时精确测量中子星的质量和转动惯量，能帮助人们进一步限定超子参数。In the framework of the relativistic mean field theory(RMFT) with GL91 cets, the momentum of inertia (I) of slowly rotating neutron stars is studied by perturbative approach. The scalar hyperon coupling should lie in the range of X_σ=0.59~1.0 to be compatible with massive neutron stars. As X_σ increases from 0.59 to 1.0, the maximum momentum of inertia(I_max) of neutron (protoneutron) stars increases by 89% (60%). According to the data of Crab, the maximum energy loss(dE/dt) of neutron (protoneutron) stars will increase by 44%(25%)and the maximum magnetic field (B) will increase by 48%(38%). I and dE/dt of PSR J0348+0432 both increase by 14%, while B decreases by 10% as X_σ increases from 0.59 to 1.0. So if the upper bound of I, or the accurate values of both the mass and I of neutron stars could be provided by the astronomical observations, the hyperon couplings should be further constrained in the future.

Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?

In the framework of the relativistic mean field theory(RMFT) with GL91 cets, the momentum of inertia (I) of slowly rotating neutron stars is studied by perturbative approach. The scalar hyperon coupling should lie in the range of X_σ=0.59~1.0 to be compatible with massive neutron stars. As X_σ increases from 0.59 to 1.0, the maximum momentum of inertia(I_max) of neutron (protoneutron) stars increases by 89% (60%). According to the data of Crab, the maximum energy loss(dE/dt) of neutron (protoneutron) stars will increase by 44%(25%)and the maximum magnetic field (B) will increase by 48%(38%). I and dE/dt of PSR J0348+0432 both increase by 14%, while B decreases by 10% as X_σ increases from 0.59 to 1.0. So if the upper bound of I, or the accurate values of both the mass and I of neutron stars could be provided by the astronomical observations, the hyperon couplings should be further constrained in the future.