对两种基于广义相对论的计算旋转中子星性质的数值方法: Hartle法和Butterworth和Ipser法(简记为BI法)进行了较详细的介绍、讨论和比较.对基于不同物态方程给出的旋转中子星的性质进行对比, 结果表明两种方法给出的相关结果例如旋转中子星的质量、半径和形变等基本一致, 特别是在观测值范围内的计算等均能较好地解释观测结果.
Two numerical schemes of rotational neutron star based on general relativity, Hartle code and Butterworth and Ipser's code(BI code), are introduced and discussed. The numerical results of the two codes with different equations of state(EOSs) are compared, and the results indicate that most properties of rotational neutron star with different EOSs and different numerical schemes are in accordance with each other.
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