g-mode of neutron stars in pseudo-Newtonian gravity

被引：1
作者：
Li, Hong-Bo [1 ,2 ]
Gao, Yong [1 ,2 ]
Shao, Lijing [2 ,3 ]
Xu, Ren-Xin [1 ,2 ]
机构：
[1] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China
[2] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China
[3] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
来源：
PHYSICAL REVIEW D | 2023年 / 108卷 / 06期
基金：
国家重点研发计划; 中国国家自然科学基金;
关键词：
EQUATION-OF-STATE; NONRADIAL OSCILLATIONS; RELATIVISTIC REGIME; GRAVITATIONAL-WAVES; HYDRODYNAMICS;
D O I：
10.1103/PhysRevD.108.064005
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The equation of state (EOS) of nuclear dense matter plays a crucial role in many astrophysical phenomena associated with neutron stars (NSs). Fluid oscillations are one of the most fundamental properties therein. NSs support a family of gravity g-modes, which are related to buoyancy. We study the gravity g-modes caused by composition gradient and density discontinuity in the framework of pseudoNewtonian gravity. The mode frequencies are calculated in detail and compared with Newtonian and general-relativistic (GR) solutions. We find that the g-mode frequencies in one of the pseudo-Newtonian treatments can approximate remarkably well the GR solutions, with relative errors in the order of 1%. Our findings suggest that, with much less computational cost, pseudo-Newtonian gravity can be utilized to accurately analyze oscillation of NSs constructed from an EOS with a first-order phase transition between nuclear and quark matter, as well as to provide an excellent approximation of GR effects in core-collapse supernova (CCSN) simulations.
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页数：15
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