Neutron Stars and the EOS
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.
Cite
@article{arxiv.1307.0397,
title = {Neutron Stars and the EOS},
author = {Madappa Prakash},
journal= {arXiv preprint arXiv:1307.0397},
year = {2013}
}
Comments
8 pages, 4 figures, 8th International Workshop on Critical Point and Onset of Deconfinement, To appear in Proceedings of Science