Realistic anisotropic neutron stars: Pressure effects

被引：14

作者：

Becerra, L. M. ^{[1
]}

Becerra-Vergara, E. A. ^{[1
]}

Lora-Clavijo, F. D. ^{[1
]}

机构：

[1] Univ Ind Santander, Escuela Fis, Grp Invest Relatividad & Gravitac, A A 678, Bucaramanga 680002, Colombia

来源：

PHYSICAL REVIEW D | 2024年 / 109卷 / 04期

关键词：

EQUATION-OF-STATE; NUCLEAR-EQUATION; PROTO-NEUTRON; SPHERES; MODELS; MATTER; FLUID; PARAMETRIZATION; FORCES; MASSES;

D O I：

10.1103/PhysRevD.109.043025

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this paper, we study the impact of anisotropy on neutron stars with different equations of state, which have been modeled by a piecewise polytropic function with continuous sound speed. Anisotropic pressure in neutron stars is often attributed to interior magnetic fields, rotation, and the presence of exotic matter or condensates. We quantify the presence of anisotropy within the star by assuming a quasilocal relationship. We find that the radial and tangential sound velocities constrain the range of anisotropy allowed within the star. As expected, the anisotropy affects the macroscopic properties of stars, and it can be introduced to reconcile them with astrophysical observations. For instance, the maximum mass of anisotropic neutron stars can be increased by up to 15% compared to the maximum mass of the corresponding isotropic configuration. This allows neutron stars to reach masses greater than 2.5M circle dot, which may explain the secondary compact object of the GW190814 event. Additionally, we propose a universal relation for the binding energy of an anisotropic neutron star as a function of the star's compactness and the degree of anisotropy.

引用

页数：11

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