Equation of state and neutron star properties constrained by nuclear physics and observation

TL;DR

This paper combines nuclear physics calculations and recent neutron star observations to constrain the equation of state of neutron-rich matter, impacting neutron star structure and properties.

Contribution

It provides new constraints on the neutron star equation of state using chiral effective field theory and observational data, with detailed numerical tables for astrophysical use.

Findings

Robust range for neutron star radii

Constraints on crust-core transition density

Impact on nuclear symmetry energy

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.