Constraining properties of massive neutron star through R-mode
Constraining properties of massive neutron star through R-mode
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DOI：
10.1140/epja/s10050-022-00781-z
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发表时间：
2022-07
期刊：
影响因子：
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通讯作者：
Jue Wang;Shengxu Yang;Dehua Wen
中科院分区：
文献类型：
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作者：
Jue Wang;Shengxu Yang;Dehua Wen
以GW190814事件为线索，在旋转中子星星的框架下，利用RNS程序研究了2.5超大质量中子星星沿着1.4正则中子星星的r模.我们的结论进一步证实了GW 190814的次级星星是一颗r模稳定态的快速旋转超大质量中子星星的可能性。对于自旋频率固定的超快旋转中子星星，其质量下限可以由r模下的临界自旋频率来约束。由于物态方程的依赖性，如果将来能观测到具有很高自旋频率的中子星星的质量，那么超致密核物质的物态方程可以通过比较不同的物态方程来约束。最后探讨了壳核跃迁密度对中子星r模的影响。
Taking the GW190814 event as a clue, r-mode of 2.5supermassive neutron star along with 1.4canonical neutron star is investigated by using RNS code in the framework of rotating neutron star. Our conclusion further confirms that for the secondary star of GW190814, there exists a possibility that it is a rapid rotating supermassive neutron star in r-mode stable state. For super fast rotating neutron star with fixed spin frequency, the lower limit of its masscan be constrained by the critical spin frequency under r-mode. As theis EOS (equation of state) dependent, if the mass of neutron star with very high spin frequency can be observed in the future, the EOS of super-dense nuclear matter can be constrained by comparing theof different EOSs. At last, the effect of crust-core transition densities on r-modes of neutron stars is explored and discussed.