Existence of quark stars in gravity's rainbow: the significance of strongly interacting quark matter*

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Abstract
This study explores the internal composition and equation of state (EoS) of quark stars (QSs) characterized by pressure anisotropy, considering recent astrophysical findings within the framework of gravity's rainbow. By employing perturbative quantum chromodynamics corrections and the concept of color superconductivity, the EoS is formulated as a dimensionless function reliant on a single parameter, thereby offering an in-depth analysis of the effects of strong interactions. The study is further extended by rescaling the EoS and applying dimensionless variables, thus covering the range from non-interacting quark matter to extreme stiffness characterized by a parameter . We also show that including the fluid anisotropy permits a stiffer EoS, facilitating the modeling of configurations that adequately meet observational constraints. We then use the supposed EoSs to numerically solve the modified Tolman-Oppenheimer-Volkoff equations and examine the effects of anisotropy and rainbow parameters on star mass, radius, and compactness. The study also explores the static stability, adiabatic index, and sound velocity profiles, thoroughly explaining QS behavior. Overall, this study offers valuable insights into the characteristics of QSs and their consistency with observational data, providing a comprehensive analysis of their EoS and internal structure.

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