EoS's of different phases of dense quark matter

TL;DR

This paper reviews how the equations of state for dense quark matter in compact stars are influenced by different phases, magnetic fields, and their impact on mass-radius relationships, constrained by recent pulsar observations.

Contribution

It provides a comprehensive review of the effects of various phases and magnetic fields on the equations of state of dense quark matter and their implications for neutron star properties.

Findings

Quark phases can significantly alter the equation of state.

Magnetic fields influence the phase structure and EoS of dense quark matter.

Mass-radius relationships are sensitive to the phase characteristics and magnetic effects.

Abstract

Compact stars with significant high densities in their interiors can give rise to quark deconfined phases that can open a window for the study of strongly interacting dense nuclear matter. Recent observations on the mass of two pulsars, PSR J1614-2230 and PSR J0348+0432, have posed a great restriction on their composition, since their equations of state must be hard enough to support masses of about at least two solar masses. The onset of quarks tends to soften the equation of state, but due to their strong interactions, different phases can be realized with new parameters that affect the corresponding equations of state and ultimately the mass-radius relationships. In this paper I will review how the equation of state of dense quark matter is affected by the physical characteristics of the phases that can take place at different baryonic densities with and without the presence of a magnetic field, as well as their connection with the corresponding mass-radius relationship, which can be derived by using different models.