For neutron matter with M-S interaction, the critical density of the ferromagnetic transition, the equation of state and the neutron star models are calculated.
还计算了在M - S势作用下的中子物质出现铁磁相变的临界密度、含有铁磁相变的物态方程及中子星模型。
We discover that it is hard for us to distinguish different neutron star models by the simple constraints of masses, redshifts and rotations on mass-radius relations.
结果发现，质量、红移及旋转频率对相应状态方程质量-半径关系的简单限制很难区分不同的中子星模型。
We discover that it is hard for us to distinguish different neutron star models by the simple constraints of masses, redshifts and rotations on mass-radius relations.
结果发现，质量、红移及旋转频率对相应状态方程质量-半径关系的简单限制很难区分不同的中子星模型。
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