Color-flavor locked quark stars in energy-momentum squared gravity

TL;DR

This paper investigates the structure of color-flavor-locked quark stars within energy-momentum squared gravity, deriving hydrostatic equilibrium and numerically solving for mass-radius relations to understand their properties.

Contribution

It introduces a novel analysis of CFL strange stars in EMSG, deriving equilibrium equations and numerically exploring their mass-radius characteristics.

Findings

EMSG modifies the structure equations of CFL strange stars.

Numerical solutions provide mass-radius relations for these stars.

Results suggest EMSG can address high-density issues without new fluid components.

Abstract

Several attempts have been made in the past decades to search for the true ground state of the dense matter at sufficiently large densities and low temperatures via compact astrophysical objects. Focusing on strange stars, we derive the hydrostatic equilibrium assuming a maximally symmetric phase of homogeneous superconducting quark matter called the \textit{color-flavor-locked} (CFL) phase in the background of energy-momentum squared gravity (EMSG). Theoretical and experimental investigations show that strange quark matter (SQM) in a CFL state can be the true ground state of hadronic matter at least for asymptotic densities, and even if the unequal quark masses. Motivated by these theoretical models, we explore the structure of stellar objects in recently proposed EMSG, which allows a correction term $T_{\mu \nu}T^{\mu \nu}$ in the action functional of the theory. Interestingly, EMSG may be effective to resolve the problems at high energy densities, e.g., relevant to the early universe and dense compact astrophysical objects without invoking some new forms of fluid stress, such as bulk viscosity or scalar fields. Finally, we solve the complicated field equations numerically to obtain the mass-radius relations for strange stars in CFL equation of state.