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Neutron Stars and the EOS

Name: Neutron Stars and the EOS
Creator: Madappa Prakash
Keywords: Nuclear Theory (nucl-th), Astrophysics - Solar and Stellar Astrophysics, Nuclear Theory, 13. Climate action, 0103 physical sciences, FOS: Physical sciences, 7. Clean energy, 01 natural sciences, Solar and Stellar Astrophysics (astro-ph.SR)

descriptionPublicationkeyboard_double_arrow_right Article , Preprint , Other literature type 13 Sep 2013Embargo end date: 01 Jan 2013Publisher:Sissa MedialabJournal:Proceedings of 8th International Workshop on Critical Point and Onset of Deconfinement — PoS(CPOD 2013)

Authors: Madappa Prakash;

doi: 10.22323/1.185.0024 , 10.48550/arxiv.1307.0397

arXiv: http://arxiv.org/abs/1307.0397

Neutron Stars and the EOS

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Abstract

Implications of recently well-measured neutron star masses, particularly near and above 2 solar masses, for the equation of state (EOS) of neutron star matter are highlighted. Model-independent upper limits to thermodynamic properties in neutron stars, which only depend on the neutron star maximum mass, established from causality considerations are presented. The need for non-perturbative treatments of quark matter in neutron stars is stressed through studies of self-bound quark matter stars, and of nucleon-quark hybrid stars. The extent to which several well-measured masses and radii of individual neutron stars can establish a model-independent EOS through an inversion of the stellar structure equations is briefly discussed.

8 pages, 4 figures, 8th International Workshop on Critical Point and Onset of Deconfinement, To appear in Proceedings of Science

Related Organizations

University System of Ohio
United States
Ohio University
United States
Department of Physics and Astronomy
United States
Ohio University - Lancaster
United States

Keywords

Nuclear Theory (nucl-th), Astrophysics - Solar and Stellar Astrophysics, Nuclear Theory, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)

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