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We present a stable model for quark stars in Rastall-Rainbow (R-R) gravity.The structure of this configuration is obtained by utilizing an interactingquark matter equation of state. The R-R gravity theory is developed as acombination of two distinct theories, namely, the Rastall theory and thegravity's rainbow formalism. Depending on the model parameters ($\bar{\lambda},\eta, \Sigma$), the mass-radius relations are numerically computed for modifiedTolman-Oppenheimer-Volkoff (TOV) equations with proper boundary conditions. Thestability of equilibrium configuration has been checked through the staticstability criterion, adiabatic index and the sound velocity. Our calculationspredict larger maximum masses for quark stars, and the obtained results arecompatible with accepted masses and radii values, including constraints fromGW190814 and GW170817 events in all the studied cases.

Investigating Stable Quark Stars in Rastall-Rainbow Gravity and Their Compatibility with Gravitational Wave Observations