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Neutron Stars 1

Equation of State and Structure

  • Textbook
  • © 2007

Overview

Editors:
  1. P. Haensel

    1. Nicholaus Copernicus Astronomical Center, Warszawa, Poland

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  2. A. Y. Potekhin

    1. Ioffe Physico-Technical Institute, St. Petersburg, Russia

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  3. D. G. Yakovlev

    1. Ioffe Physico-Technical Institute, St. Petersburg, Russia

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Part of the book series: Astrophysics and Space Science Library (ASSL, volume 326)

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Table of contents (9 chapters)

  1. Front Matter

    Pages i-xxiii
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  2. Overview

    Pages 1-51

  3. Equilibrium Plasma Properties. Outer Envelopes

    Pages 53-114

  4. Structure and Equation of State of Neutron Star Crusts

    Pages 115-165

  5. Envelopes with Strong Magnetic Fields

    Pages 167-205

  6. Neutron Star Cores: Nucleons and Hyperons

    Pages 207-280

  7. Neutron Star Structure

    Pages 281-349

  8. Neutron Stars with Exotic Cores

    Pages 351-405

  9. Strange Matter and Strange Stars

    Pages 407-454

  10. Theory Versus Observations

    Pages 455-516

  11. Back Matter

    Pages 517-619
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Keywords

About this book

Neutron stars play a unique role in physics and astrophysics. On the one hand, they contain matter under extreme physical conditions, and their theories are based on risky and far extrapolations of what we consider reliable physical theories of the structure of matter tested in laboratory. On the other hand, their observationsoffertheuniqueopportunitytotestthesetheories. Moreover, n- tronstarsareimportantdramaticpersonaeonthestageofmodernastrophysics; they participate in many astronomical phenomena. ?3 Neutronstarscontainthematterofdensityrangingfromafew g cm attheir 15 ?3 surface, where the pressure is small, to more than 10 gcm at the center, 36 ?2 wherethepressureexceeds10 dyncm . Tocalculateneutronstarstructure, one needs the dependence of the pressure on density, the so called equation of state (EOS), in this huge density range, taking due account of temperature, 9 more than10 K in young neutron stars, and magnetic ?elds, sometimes above 15 10 G. The present book is mainly devoted to the theory of the EOS of neutron star matter and its consequences for neutron star structure. As one moves from the neutron star surface to the center, the methods to calculate the EOS change. Atomic structure and plasma theories are used for the surface stellar layers. Deeper layers of the neutron star crust require nuclear theory combined with plasma physics, both in very exotic density-temperature regimes. Finally, the neutron star core necessitates many-body theory of dense strongly interacting systems,togetherwiththephysicsofstronginteractionsofelementaryparticles.

Editors and Affiliations

  • Nicholaus Copernicus Astronomical Center, Warszawa, Poland

    P. Haensel

  • Ioffe Physico-Technical Institute, St. Petersburg, Russia

    A. Y. Potekhin, D. G. Yakovlev

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