Equation of state and neutron star properties constrained by nuclear physics and observation
Abstract
Microscopic calculations of neutron matter based on nuclear interactions derived from chiral effective field theory, combined with the recent observation of a 1.97 +- 0.04 M_sun neutron star, constrain the equation of state of neutron-rich matter at sub- and supranuclear densities. We discuss in detail the allowed equations of state and the impact of our results on the structure of neutron stars, the crust-core transition density, and the nuclear symmetry energy. In particular, we show that the predicted range for neutron star radii is robust. For use in astrophysical simulations, we provide detailed numerical tables for a representative set of equations of state consistent with these constraints.
Keywords
Cite
@article{arxiv.1303.4662,
title = {Equation of state and neutron star properties constrained by nuclear physics and observation},
author = {K. Hebeler and J. M. Lattimer and C. J. Pethick and A. Schwenk},
journal= {arXiv preprint arXiv:1303.4662},
year = {2013}
}
Comments
35 pages, 12 figures, NORDITA preprint 2013-22