Structure of ultra-magnetised neutron stars

被引：12

作者：

Chatterjee, Debarati ^{[1
]}

Novak, Jerome ^{[2
]}

Oertel, Micaela ^{[2
]}

机构：

[1] Pune Univ Campus, Inter Univ Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India

[2] Univ Paris, CNRS, Univ PSL, Observ Paris,LUTH, F-92195 Meudon, France

来源：

EUROPEAN PHYSICAL JOURNAL A | 2021年 / 57卷 / 08期

关键词：

EQUATION-OF-STATE; ADIABATIC STABILITY; EQUILIBRIUM-MODELS; RELATIVISTIC STARS; FIELD DISTRIBUTION; NUCLEAR-MATTER; CRUST; PULSARS; SUSCEPTIBILITY; TRANSITION;

D O I：

10.1140/epja/s10050-021-00525-5

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

In this review we discuss self-consistent methods to calculate the global structure of strongly magnetised neutron stars within the general-relativistic framework. We outline why solutions in spherical symmetry cannot be applied to strongly magnetised compact stars, and elaborate on a consistent formalism to compute rotating magnetised neutron star models. We also discuss an application of the above full numerical solution for studying the influence of strong magnetic fields on the radius and crust thickness of magnetars. The above technique is also applied to construct a "universal" magnetic field profile inside the neutron star, that may be useful for studies in nuclear physics. The methodology developed here is particularly useful to interpret multi-messenger astrophysical data of strongly magnetised neutron stars.

引用

页数：15

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