Non-singular anisotropic hybrid star model in f(ℛ,𝒜) theory of gravity

The objective of this study is to explore the characteristics of a stationary, anisotropic, relativistic hybrid compact star consisting of quark matter (QM) at its core and ordinary baryonic matter (OBM) in its crust. To model the stellar system, separate equations of state (EoSs) are employed for each matter component. The quark matter is characterized using the MIT bag model equation of state, expressed as [Formula: see text], which establishes the relationship between the quark matter’s pressure and density inside the star. Additionally, for the baryonic matter, a simplified linear equation of state [Formula: see text] is applied to connect the radial pressure and matter–density. The configuration of the star is formulated within the context of [Formula: see text] gravity, where a linear association between the Ricci tensor [Formula: see text] and the anticurvature scalar [Formula: see text] is incorporated. To address the field equations within this modified gravitational framework, we employ the Krori and Barua method to derive the metric potentials. The feasibility of the proposed model is assessed through a graphical analysis, ensuring the fulfillment of physically realistic conditions. Our investigation centers on the compact star LMC X-4, characterized by the parameters [Formula: see text] and [Formula: see text], making it a strong candidate for a strange quark star. To confirm the physical viability of the model, we evaluate several essential criteria, including dynamical equilibrium, energy conditions, the compactness factor, the mass function, and the surface redshift. The obtained results affirm the robustness of the hybrid star model under study.

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