Neutron stars and the equation of state

被引：1

作者：

Schramm, S. ^{[1
]}

Dexheimer, V. ^{[2
]}

Mukherjee, A. ^{[1
]}

Steinheimer, J. ^{[1
]}

机构：

[1] FIAS, D-60438 Frankfurt, Germany

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

来源：

JOURNAL OF ASTROPHYSICS AND ASTRONOMY | 2018年 / 39卷 / 04期

关键词：

Neutron stars; equation of state; hyper stars; hybrid stars; NUCLEAR; LATTICE; MATTER;

D O I：

10.1007/s12036-018-9534-5

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The interior of neutron stars consists of the densest, although relatively cold, matter known in the universe. Here, baryon number densities might reach values close to ten times the nuclear saturation density. These suggest that the constituents of neutron star cores not only consist of nucleons, but also of more exotic baryons like hyperons or a phase of deconfined quarks. We discuss the consequences of such exotic particles on the gross properties and phenomenology of neutron stars. In addition, we determine the general phase structure of dense and also hot matter in the chiral parity-doublet model and confront model results with the recent constraints derived from the neutron star merger observation.

引用

页数：8

共 39 条

[11]

Fodor Z, 2004, J HIGH ENERGY PHYS, DOI 10.1088/1126-6708/2004/04/050

[12] Neutron stars with hyperon cores: stellar radii and equation of state near nuclear density [J].