Influence of the hadronic equation of state on the hadron-quark phase transition in neutron stars

TL;DR

This paper investigates how the hadronic equation of state affects the hadron-quark phase transition within neutron stars, using RMF and NJL models to analyze the conditions for mixed phases and quark cores.

Contribution

It introduces a combined RMF and NJL modeling approach to study the influence of hadronic EoS on neutron star phase transitions and core composition.

Findings

Neutron stars have a large hyperon population but no pure quark core.

The existence of a mixed phase depends on RMF parameters.

Pure quark cores are unlikely due to insufficient density.

Abstract

We study the hadron-quark phase transition in the interior of neutron stars. The relativistic mean field (RMF) theory is adopted to describe the hadronic matter phase, while the Nambu-Jona-Lasinio (NJL) model is used for the quark matter phase. The influence of the hadronic equation of state on the phase transition and neutron star properties are investigated. We find that a neutron star possesses a large population of hyperons, but it is not dense enough to possess a pure quark core. Whether the mixed phase of hadronic and quark matter exist in the core of neutron stars depends on the RMF parameters used.