Equation of state, neutron stars and exotic phases

被引：27
作者：
Lattimer, James M. [1 ]
Prakash, Madappa [1 ]
机构：
[1] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA
来源：
NUCLEAR PHYSICS A | 2006年 / 777卷
关键词：
neutron stars; equation of state;
D O I：
10.1016/j.nuclphysa.2005.01.014
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：
The role of the equation of state in the structure of neutron stars is summarized. At densities beyond a few times the normal nuclear saturation density, the neutron-proton-electron sea can be supplemented with more exotic matter, usually involving strangeness, such as hyperons, kaon or pion condensates, and deconfined quark matter. In the case of a boson condensate or deconfined quark matter, the exotic matter may form a mixed-phase region with the hadronic matter. Global aspects of neutron stars, such as radii, moments of inertia and the maximum mass, can be related to specific properties of matter at selected density ranges. Recent observations of isolated neutron stars and pulsars in binaries are beginning to yield significant constraints on structural properties of neutron stars and hence on the properties and composition of neutron-rich nuclear matter. (c) 2005 Published by Elsevier B.V.
引用
收藏
页码：479 / 496
页数：18
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