Equation of state at neutron-star densities and beyond from perturbative QCD

TL;DR

This paper investigates how perturbative QCD constraints influence the neutron-star dense matter equation-of-state, highlighting the importance of the termination density and introducing a new QCD likelihood function that reduces this sensitivity.

Contribution

It introduces a new QCD likelihood function that incorporates additional calculations and minimizes dependence on the termination density in EOS inference.

Findings

EOS modeling is highly sensitive to the termination density.

A new QCD likelihood function reduces this sensitivity.

Explicit modeling connects perturbative QCD densities to neutron-star matter.

Abstract

We explore the consequences of imposing robust thermodynamic constraints arising from perturbative Quantum Chromodynamics (QCD) when inferring the dense-matter equation-of-state (EOS). We find that the termination density, up to which the EOS modeling is performed in an inference setup, strongly affects the constraining power of the QCD input. This sensitivity in the constraining power arises from EOSs that have a specific form, with drastic softening immediately above the termination density followed by a strong stiffening. We also perform explicit modeling of the EOS down from perturbative-QCD densities to construct a new QCD likelihood function that incorporates additional perturbative-QCD calculations of the sound speed and is insensitive to the termination density, which we make publicly available.