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Equations of State of Neutron Star Matter

  • Koutarou Kyutoku
Chapter
Part of the Springer Theses book series (Springer Theses)

Abstract

The purpose of this thesis is to investigate dependence of gravitational waves on the NS EOS, aiming for determining or at least constraining the EOS at high density above the nuclear saturation density \(\varvec{\rho }_{\mathrm{sat }} \approx 2.7 \times 10^{14} \, \mathrm{g \, cm^{-3} }\) (or \(n_{\mathrm{sat }} \approx 0.16 \, \mathrm{fm }^{-3}\) in terms of the baryon number density) by gravitational-wave observation. Here, we mean “cold, zero-temperature EOS” by “EOS,” because the finite-temperature effect is believed to have a negligible role in determining the property of an isolated NS and a NS just before the merger [1]. In this chapter, we review relations between the NS properties and the NS EOS from a theoretical point of view, as well as describe how the NS EOS is constrained by current astrophysical observation based on electromagnetic radiation. Finally, we describe our model of the cold, zero-temperature EOS, i.e., the piecewise polytropic EOS [2], adopted in this thesis

Keywords

Newtonian Gravity Gravitational Redshift Direct URCA Process Nuclear Saturation Density Photospheric Radius 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer Japan 2013

Authors and Affiliations

  1. 1.KEK, Cosmophysics GroupInstitute of Particle and Nuclear StudiesIbarakiJapan

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