Equation of state in hybrid stars and the stability window of quark matter

TL;DR

This paper investigates the properties and stability of hybrid stars with mixed phases of nuclear and strange quark matter, using a quark quasiparticle model to analyze their equations of state and mass-radius relations.

Contribution

It introduces a detailed analysis of the stability windows of strange quark matter and their impact on hybrid star properties using a self-consistent quark quasiparticle model.

Findings

Quark-hadron mixed phases are linked to meta-stable or unstable pure quark matter regions.

The mass of hybrid stars is reduced to about 1.64 solar masses with a radius of 10.6 km.

The equation of state of quark matter dominates the mass-radius relation of hybrid stars.

Abstract

Properties of hybrid stars with a mixed phase composed of asymmetric nuclear matter and strange quark matter are studied. The quark phase is investigated by the quark quasiparticle model with a self-consistent thermodynamic and statistical treatment. We present the stability windows of the strange quark matter with respect to the interaction coupling constant versus the bag constant. We find that the appearance of the quark-hadron mixed phases is associated with the meta-stable or unstable regions of the pure quark matter parameters. The mass-radius relation of the hybrid star is dominated by the equation of state of quark matter rather than nuclear matter. Due to the appearance of mixed phase, the mass of hybrid star is reduced to 1.64 M$_{\odot}$ with radius 10.6 km by comparison with neutron star.