The Deconfinement Phase Transition in Proto-Neutron-Star Matter

TL;DR

This paper investigates the deconfinement phase transition in hot, dense nuclear matter within proto-neutron stars using the Chiral Mean Field model, analyzing phase mixtures and comparing with perturbative QCD data.

Contribution

It applies the CMF model to study phase transitions in proto-neutron-star matter, considering various phase mixtures and conserved quantities, and compares results with PQCD data.

Findings

Identification of phase transition characteristics in proto-neutron-star matter

Analysis of phase mixtures with conserved quantities

Comparison of model results with perturbative QCD data

Abstract

In this work, we study in detail the deconfinement phase transition that takes place in hot/dense nuclear matter in the context of neutron stars and proto-neutron stars (in which lepton fraction is fixed). The possibility of different mixtures of phases with different locally and globally conserved quantities is considered in each case. For this purpose, the Chiral Mean Field (CMF) model, an effective relativistic model that includes self-consistent chiral symmetry restoration and deconfinement to quark matter, is employed. Finally, we compare our results with data provided by PQCD for different temperatures and conditions.