Analyzing stability of charged anisotropic configurations of dark energy stars in Rastall gravity

This paper establishes two distinct solutions for dark energy stars, representing charged spherical configurations within the framework of Rastall gravity. The modified field equations are formulated by considering a static spherically symmetric interior geometry. By using two particular equations of state linking dark energy components with the ordinary matter, we obtain solutions to the field equations. As the system has more unknowns and fewer equations, we use two different models such as Finch–Skea and Tolman IV ansatz to obtain unique solutions. We then use junction conditions at the star’s boundary to calculate the constants for each solution. A class of specific physical conditions are then imposed to check whether the generated models are physically existing. Furthermore, the observed data of a known star 4U 1538-52, along with a range of Rastall parametric values and two distinct charge choices, are employed to graphically evaluate the proposed models. Our analysis concludes that both stellar models meet the necessary criteria for physical viability for specific parametric values.