Internal composition of proto-neutron stars under strong magnetic fields

被引：20

作者：

Franzon, B. ^{[1
]}

Dexheimer, V. ^{[2
]}

Schramm, S. ^{[1
]}

机构：

[1] Frankfurt Inst Adv Studies, Ruth Moufang 1, D-60438 Frankfurt, Germany

[2] Kent State Univ, Dept Phys, Kent, OH 44242 USA

来源：

PHYSICAL REVIEW D | 2016年 / 94卷 / 04期

关键词：

MAGNETOROTATIONAL INSTABILITY; DIFFERENTIAL ROTATION; ADIABATIC STABILITY; EQUILIBRIUM-MODELS; RELATIVISTIC STARS; GENERAL-RELATIVITY; COLLAPSE; CORE; EVOLUTION; EQUATIONS;

D O I：

10.1103/PhysRevD.94.044018

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this work, we study the effects of magnetic fields and rotation on the structure and composition of proto-neutron stars. A hadronic chiral SU(3) model is applied to cold neutron stars and proto-neutron stars with trapped neutrinos and at fixed entropy per baryon. We obtain general relativistic solutions for neutron and proto-neutron stars endowed with a poloidal magnetic field by solving Einstein-Maxwell field equations in a self-consistent way. As the neutrino chemical potential decreases in value over time, this alters the chemical equilibrium and the composition inside the star, leading to a change in the structure and in the particle population of these objects. We find that the magnetic field deforms the star and significantly alters the number of trapped neutrinos in the stellar interior, together with strangeness content and temperature in each evolution stage.

引用

页数：12

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