Dark energy stars modeling in f(𝕋) gravity via Finch–Skea model

Dark energy is the most abundant component in the current universe and is responsible for its rapid expansion. In this paper, we expand the notion of a dark energy star, which is composed of ordinary and dark matter, within the context of [Formula: see text] theory, an extension of teleparallel gravity in which gravity is defined by torsion contrary to curvature. We develop the model in the Finch–Skea space-time configuration within [Formula: see text] gravity, presuming that the dark energy density corresponds to the isotropic ideal fluid matter density. Here, we investigate the effects of dark energy, via employing torsion impacts, on star mass, equilibrium, and compactness, among other factors. The stability of the star structure is thoroughly examined, together with physical properties of the model, including mass function, pressure, density, surface redshift, etc. Using the M–R diagram, we were able to determine the maximum permissible mass from our model. The model founded on [Formula: see text] is singularity-free, behaves physically realistic, and meets all energy criteria. We examined a number of the model’s physical characteristics to ensure that it satisfies all regularity requirements, is stable, and so physically plausible.

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