Modeling anisotropic dark energy self-gravitating stars satisfying the Karmarkar condition

This article introduces a simplified model of static, spherical stellar systems interacting with anisotropic dark energy, using the Buchdahl model as the background metric potential. The notion of cosmic dark energy may serve as a potential mechanism to counteract the relativistic gravitational collapse of stellar distributions into singularities. Dark energy plays a vital role in shaping the cosmos on the largest scales, as it is the driving force behind the observed accelerated expansion. Therefore, it is reasonable to think that dark energy influences the kinematics of gravitationally bound stellar structures (Sakti and Sulaksono, 2021) [65]. Motivated by this, we introduce a self-gravitating stellar system model under the influence of dark energy, which incorporates both dark and ordinary matter. The model assumes a direct proportionality between the dark energy density and the perfect fluid density. We will then analyze the astrophysical features, including the regularity of the metric variables, density, pressure, mass–radius relationship, stability, dark energy parameters, and equilibrium conditions associated with the model. The model is promising due to its adherence to energy conditions and lack of a central singularity. By examining a mass–radius diagram, we have found the maximum mass limit for this type of star. Our results show that our suggested model corresponds to a feasible and physically realistic star structure that satisfies all stability criteria.