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Neutron stars 1 : equation of state and structure

著者: Paweł Haensel; A Y Potekhin; D G Yakovlev
出版商: New York, N.Y. : Springer, 2007.
丛书: Astrophysics and space science library, v. 326.
版本/格式:   Print book : 英语查看所有的版本和格式
数据库:WorldCat
提要:
"With masses comparable to that of the Sun and radii of about only ten kilometers, neutron stars are the most compact stars in the Universe. They offer a unique possibility of revealing the properties of superdense matter through a comparison of theoretical models to observations. This book describes all layers of neutron stars with the emphasis on their thermodynamics and composition. Theories of dense matter are  再读一些...
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所有的著者/提供者: Paweł Haensel; A Y Potekhin; D G Yakovlev
ISBN: 0387335439 9780387335438 1441922148 9781441922144
OCLC号码: 272564139
描述: xxiii, 619 pages : illustrations ; 25 cm.
内容: Overview.- Equilibrium Plasma Properties. Outer Envelopes.- Structure and Equation of State of Neutron Star Crusts.- Envelopes with Strong Magnetic Fields.- Neutron Star Cores: Nucleons and Hyperons.- Neutron Star Structure.- Neutron Stars with Exotic Cores.- Strange Matter and Strange Stars.- Theory Versus Observations.
丛书名: Astrophysics and space science library, v. 326.
责任: P. Haensel, A.Y. Potekhin, and D.G. Yakovlev.
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摘要:

The book gives an extended review of theoretical and observational aspects of neutron star physics. It describes all layers of neutron stars, from the surface to the core, with the emphasis on their  再读一些...

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   schema:reviewBody ""With masses comparable to that of the Sun and radii of about only ten kilometers, neutron stars are the most compact stars in the Universe. They offer a unique possibility of revealing the properties of superdense matter through a comparison of theoretical models to observations. This book describes all layers of neutron stars with the emphasis on their thermodynamics and composition. Theories of dense matter are reviewed and used to construct neutron star models. Separate chapters are devoted to hypothetical strange quark stars and exotic phases of dense matter in neutron star cores. The effects of strong magnetic fields in neutron star envelopes are discussed and the final chapter compares neutron star models to observations. Book jacket."--Jacket." ;
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