Phase Transitions in Rotating Neutron Stars: Effects of Stellar Crusts
Phase Transitions in Rotating Neutron Stars: Effects of Stellar Crusts
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DOI：
10.1086/324330
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发表时间：
2002-01
期刊：
影响因子：
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通讯作者：
K. Cheng;Y. Yuan;Jun-Long Zhang
中科院分区：
文献类型：
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作者：
K. Cheng;Y. Yuan;Jun-Long Zhang
快速旋转的中子星由于失去角动量而自旋下降，其中心密度增加，核心核物质转化为夸克物质，导致恒星转动惯量急剧减小，甚至导致脉冲星进入自旋上升时代（Glendenning, Pei, & Weber 1997）。我们发现，给定液核的某一状态方程，即使转动惯量作为旋转频率的函数发生反向弯曲，总转动惯量只要增加1%就能携带足够的角动量，使恒星停止自旋。总转动惯量的微小差异可能是由于地壳中亚核物质的性质不同，特别是不同模型之间固体地壳内边界的过渡密度和压力不同。背弯现象对地壳物理状态的强烈依赖，原则上提供了一种新的观测方法来检验和约束有关亚核物质的理论。
As a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central density increases and the nuclear matter in its core converts to quark matter, which leads to a drastic decrease of the stellar moment of inertia, and even results in an era of spin-up of the pulsar (Glendenning, Pei, & Weber 1997). We find that given a certain equation of state in the liquid core, even if the backbending of the moment of inertia as a function of the rotating frequency occurs, an increase of the total moment of inertia by only 1% could carry adequate angular momentum and stop the star spin-up. This small discrepancy in the total moment of inertia might be due to the different properties of subnuclear matter in the crust, especially to different transition density and pressure at the inner boundary of the solid crust between various models. The strong dependence of the phenomenon of backbending on the physical state of the crust provides, in principle, a new observational approach to check and constrain theories on subnuclear matter.