Modelling Hybrid Stars in Quark-Hadron Approaches

TL;DR

This paper explores models of hybrid stars with quark and hadron phases, analyzing their stability, the role of quark interactions, and compatibility with lattice QCD data to understand dense matter in neutron star cores.

Contribution

It compares different modeling approaches for hybrid stars and examines the impact of quark interactions on their stability and consistency with lattice QCD.

Findings

Quark interactions significantly influence hybrid star stability.

Certain models align with lattice QCD constraints.

Hybrid stars can exist with mixed hadron-quark phases.

Abstract

The density in the core of neutron stars can reach values of about 5 to 10 times nuclear matter saturation density. It is, therefore, a natural assumption that hadrons may have dissolved into quarks under such conditions, forming a hybrid star. This star will have an outer region of hadronic matter and a core of quark matter or even a mixed state of hadrons and quarks. In order to investigate such phases, we discuss different model approaches that can be used in the study of compact stars as well as being applicable to a wider range of temperatures and densities. One major model ingredient, the role of quark interactions in the stability of massive hybrid stars is discussed. In this context, possible conflicts with lattice QCD simulations are investigated.