Non-singular Anisotropic hybrid star model in the context of f(R,G) gravity

The presence of quark matter within neutron stars could give rise to profound astrophysical implications. A confirmation of this quark matter hypothesis would suggest that a new class of compact objects such as hybrid stars should form in preference to standard neutron stars. This study explores the physical characteristics of these hybrid stars, which contain both baryonic and quark matter phases, within the framework of [Formula: see text] gravity. We utilize the Kuchowicz potential to model the spacetime geometry, employing a linear equation of state for baryonic matter and the MIT bag model for the quark core. By examining the boundary conditions between the interior and the external Schwarzschild spacetime, we determine the model’s free parameters. The viability of our concept is then rigorously tested through a series of physical analyses and graphical explorations. Our results consistently indicate that the proposed system is both physically stable and well-behaved, offering strong support for the existence of hybrid stars in [Formula: see text] gravity.

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