Neutron star structure from QCD

TL;DR

This paper reviews how first-principles QCD calculations at different densities can constrain neutron star properties, achieving an accurate Equation of State by combining theoretical results with observational bounds.

Contribution

It demonstrates a method to accurately determine the neutron star Equation of State using state-of-the-art QCD calculations and observational data.

Findings

Equation of State constrained to better than 30% accuracy

Combines Chiral Effective Theory and perturbative QCD results

Provides a comprehensive framework for neutron star modeling

Abstract

In this review article, we argue that our current understanding of the thermodynamic properties of cold QCD matter, originating from first principles calculations at high and low densities, can be used to efficiently constrain the macroscopic properties of neutron stars. In particular, we demonstrate that combining state-of-the-art results from Chiral Effective Theory and perturbative QCD with the current bounds on neutron star masses, the Equation of State of neutron star matter can be obtained to an accuracy better than 30% at all densities.