Perturbative QCD reveals the softening of matter in the cores of massive neutron stars

TL;DR

This paper uses perturbative QCD calculations combined with astrophysical data to constrain the equation of state of neutron star matter, revealing a softening at high densities suggestive of phase transitions or conformal symmetry restoration.

Contribution

It introduces a novel method of applying perturbative QCD constraints to neutron star equations of state using Bayesian inference and Gaussian processes.

Findings

EoS softens at maximum neutron star densities

Constraints suggest possible phase transition or symmetry restoration

Data slightly favor the occurrence of a phase transition in massive NS cores

Abstract

The cores of neutron stars (NSs) contain the densest matter in the universe. Rapid advancements in neutron-star observations allow unprecedented empirical access to cold, ultra-dense Quantum Chromodynamics (QCD) matter. The combination of these observations with theoretical calculations has revealed previously inaccessible features of the equation of state (EoS) and the QCD phase diagram. In this thesis, I demonstrate how perturbative-QCD calculations at asymptotically high baryon densities provide robust constraints on the EoS at neutron-star densities. The method for constraint propagation is based solely on thermodynamical causality, stability, and consistency of the EoS. By constructing a large ensemble of EoSs using Gaussian processes regression and incorporating it into a Bayesian inference of EoS, I demonstrate that the novel pQCD constraints go beyond those obtained from current astrophysical observations alone, forcing the EoS to soften at the maximum densities of stable neutron stars. This softening of the EoS can be interpreted as an indication of approximate conformal symmetry restoration, a sign of a first-order phase transition (FOPT), or potentially both. I show that the conformal symmetry restoration is consistent with the hypothesis of quark matter cores inside the most massive NSs. Although current astrophysical data and theoretical inputs cannot definitively distinguish between the two scenarios, they slightly favor the occurrence of a phase transition of some kind - whether a crossover to quark matter or a destabilizing FOPT - in the cores of the most massive neutron stars.