Hybrid stars with the Dyson-Schwinger quark model

TL;DR

This paper investigates the hadron-quark phase transition in neutron stars using a microscopic hadronic model and the Dyson-Schwinger approach for quark matter, revealing conditions for hybrid star stability.

Contribution

It introduces the Dyson-Schwinger model for quark matter in neutron star studies and compares it with the MIT bag model, analyzing phase transition conditions.

Findings

Hadron-quark transition occurs only without hyperons in Dyson-Schwinger model.

Two-solar-mass hybrid stars are possible with a sufficiently stiff nucleonic EoS.

Comparison shows differences between Dyson-Schwinger and MIT bag models in phase transition predictions.

Abstract

We study the hadron-quark phase transition in the interior of neutron stars. For the hadronic sector, we use a microscopic equation of state involving nucleons and hyperons derived within the Brueckner-Hartree-Fock many-body theory with realistic two-body and three-body forces. For the description of quark matter, we employ the Dyson-Schwinger approach and compare with the MIT bag model. We calculate the structure of neutron star interiors comprising both phases and find that with the Dyson-Schwinger model, the hadron-quark phase transition takes place only when hyperons are excluded, and that a two-solar-mass hybrid star is possible only if the nucleonic equation of state is stiff enough.