\begin{document}$\bar{\lambda}$\end{document}. 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."> Existence of quark stars in gravity's rainbow: the significance of strongly interacting quark matter -
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