Hybrid protoneutron stars with the Dyson-Schwinger quark model

TL;DR

This paper investigates the phase transition from hadronic to quark matter in protoneutron stars at finite temperature using the Dyson-Schwinger model combined with the Brueckner-Hartree-Fock approach, highlighting the impact on maximum star mass.

Contribution

It introduces a hybrid model for protoneutron stars using Dyson-Schwinger and Brueckner-Hartree-Fock approaches, exploring the effects of nuclear forces and quark model parameters on star properties.

Findings

Transition occurs at high density compared to bag model.

Maximum mass exceeds two solar masses with strong three-body forces.

Hybrid stars can have larger maximum mass than cold neutron stars.

Abstract

We study the hadron-quark phase transition at finite temperature in the interior of protoneutron stars, combining the Dyson-Schwinger model for quark matter with the Brueckner-Hartree-Fock approach for hadronic matter. We discuss the dependence of the results on different nuclear three-body forces and on details of the quark model. %Compared to the bag model, the transition from the hadron phase %(without hyperons) to the quark phase appears at large density. A maximum mass exceeding two solar masses can be obtained with a strong three-body force and suitable parameter values in the Dyson-Schwinger model. With a hybrid configuration, the maximum mass of protoneutron stars is larger then that of cold neutron stars, such that a delayed collapse might be possible in principle.