Connecting Neutron Star Observations to Three-Body Forces in Neutron Matter and to the Nuclear Symmetry Energy

TL;DR

This paper demonstrates that neutron star observations significantly constrain the equation of state of neutron matter, providing insights into three-body forces and nuclear symmetry energy, with implications for theoretical models and experimental comparisons.

Contribution

It links neutron star data to the properties of neutron matter, especially the three-body force strength and symmetry energy, using phenomenological models and observational constraints.

Findings

Neutron star mass and radius measurements constrain the neutron matter equation of state.

Results are robust against variations in high-density modeling approaches.

Constraints on three-body force strength and symmetry energy are derived from astrophysical data.

Abstract

Using a phenomenological form of the equation of state of neutron matter near the saturation density which has been previously demonstrated to be a good characterization of quantum Monte Carlo simulations, we show that currently available neutron star mass and radius measurements provide a significant constraint on the equation of state of neutron matter. At higher densities we model the equation of state using polytropes and a quark matter model, and we show that our results do not change strongly upon variation of the lower boundary density where these polytropes begin. Neutron star observations offer an important constraint on a coefficient which is directly connected to the strength of the three-body force in neutron matter, and thus some theoretical models of the three-body may be ruled out by currently available astrophysical data. In addition, we obtain an estimate of the symmetry energy of nuclear matter and its slope that can be directly compared to the experiment and other theoretical calculations.