Massive Compact Stars as Quark Stars

TL;DR

This paper discusses the challenge of modeling massive quark stars that align with recent observations of high-mass compact stars, emphasizing the need for stiffer equations of state to explain their stability.

Contribution

It highlights the discrepancy between existing quark matter equations of state and the observational data, proposing the necessity for stiffer models to account for massive quark stars.

Findings

Existing quark matter equations are too soft for high-mass stars

Observations impose constraints on the equations of state

Stiffer equations are needed for stable massive quark stars

Abstract

High massive compact stars have been reported recently in the literature, providing strong constraints on the properties of the ultradense matter beyond the saturation nuclear density. In view of these results, the calculations of quark star or hybrid star equilibrium structure must be compatible with the provided observational data. But, since the used equations of state describing quark matter are in general too soft, in comparison with the equation of states used to describe the hadronic or nuclear matter, the calculated quark star models presented in the literature are in general not suitable to explain the stability of high compact massive objects.