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Abstract We propose a new hybrid stellar model whose matter distribution is characterized by two components: normal matter and strange-quark matter. The construction of this gravitationally bound hybrid star involves a complexity-free condition, which is used to derive the temporal metric function. However, for the radial metric function, the well-known Finch-Skea metric potential is considered. To elaborate on the interplay between the matter variables of the complexity-free hybrid star, we employ the popular MIT bag model. We analyze the physical effectiveness of the complexity-free hybrid astrophysical configuration by constructing closed-form analytical solutions and then performing a complete graphical analysis to capture the model’s physical features. This is achieved by considering six model stars as prospective models for strange quark-matter self-gravitating systems, such as Her X-1, SMC X-4, Vela X-1, 4U 1538-52, PSR J1614-2230, and Cen X-3. We show that the proposed hybrid stellar model is robust for accurately estimating the measured radii of the above-mentioned astrophysical configurations. In addition, several physical tests have been performed to ensure the applicability and physical consistency of the suggested model. In these tests, both analytical and graphical evaluations are included, which involve the analysis of several factors, including physically acceptable behaviors of structural variables, the equilibrium of external forces, the mass-to-radius ratio, energy bounds, gravitational redshift, and related quantities. Our findings indicate that the presented hybrid star model fulfills the required physical constraints for an astrophysically valid compact system.
Khan et al. (Thu,) studied this question.