Equation of state of hypernuclear matter and neutron stars

被引：0

作者：

Rios, A ^{[1
]}

Polls, A ^{[1
]}

Ramos, A ^{[1
]}

Vidaña, I ^{[1
]}

机构：

[1] Univ Barcelona, Dept Estructura & Constituents Mat, E-08028 Barcelona, Spain

来源：

HISPALENSIS LECTURES ON NUCLEAR PHYSICS, VOL 2 | 2004年 / 652卷

关键词：

D O I：

暂无

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：

These lectures contain a pedagogical introduction to the equation of state of nuclear matter and to the structure of neutron stars. Particular attention is devoted to the beta-equilibrium conditions and to the composition of neutron stars. The possible appearance of hyperons to reach the beta-equilibrium when the density increases is carefully analyzed. In general, the introduction of new degrees of freedom, such as for instance the hyperons, produces a softening of the equation of state and as a consequence the maximum mass of the neutron star decreases. Finally, relevant observational data are compared with microscopic predictions.

引用

页码：217 / 244

页数：28

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