Neutron Stars-Cooling and Transport

被引：227

作者：

Potekhin, Alexander Y. ^{[1
,2
,3
]}

Pons, Jose A. ^{[4
]}

Page, Dany ^{[5
]}

机构：

[1] Ioffe Inst, St Petersburg 194021, Russia

[2] Cent Astron Observ Pulkovo, St Petersburg 196140, Russia

[3] St Petersburg State Polytech Univ, St Petersburg 196140, Russia

[4] Univ Alacant, Dept Fisa Aplicada, Alacant 03080, Spain

[5] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico

来源：

SPACE SCIENCE REVIEWS | 2015年 / 191卷 / 1-4期

基金：

俄罗斯科学基金会;

关键词：

Neutron stars; Magnetic fields; Dense matter; Thermal emission; Heat transport; EQUATION-OF-STATE; X-RAY-EMISSION; QUASI-PARTICLE INTERACTIONS; STRONG MAGNETIC-FIELD; DIRECT URCA PROCESS; THERMAL-CONDUCTIVITY; NUCLEON SUPERFLUIDITY; PAIR BREMSSTRAHLUNG; TEMPERATURE DISTRIBUTION; RELATIVISTIC ELECTRON;

D O I：

10.1007/s11214-015-0180-9

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Observations of thermal radiation from neutron stars can potentially provide information about the states of supranuclear matter in the interiors of these stars with the aid of the theory of neutron-star thermal evolution. We review the basics of this theory for isolated neutron stars with strong magnetic fields, including most relevant thermodynamic and kinetic properties in the stellar core, crust, and blanketing envelopes.

引用

页码：239 / 291

页数：53

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