Constraints on neutron star radii based on chiral effective field theory interactions

TL;DR

This paper uses chiral effective field theory interactions to tightly constrain neutron star radii, integrating microscopic calculations with observational data to refine radius estimates for 1.4 solar mass neutron stars.

Contribution

It provides a more precise radius range for neutron stars by combining microscopic nuclear physics calculations with astrophysical observations.

Findings

Neutron star radius for 1.4 solar masses is constrained to 9.7-13.9 km.

Microscopic calculations reduce uncertainties in neutron-rich matter properties.

Theoretical uncertainties stem from many-body forces and high-density extrapolations.

Abstract

We show that microscopic calculations based on chiral effective field theory interactions constrain the properties of neutron-rich matter below nuclear densities to a much higher degree than is reflected in commonly used equations of state. Combined with observed neutron star masses, our results lead to a radius R = 9.7 - 13.9 km for a 1.4 M_{solar} star, where the theoretical range is due, in about equal amounts, to uncertainties in many-body forces and to the extrapolation to high densities.