Impact of equation of state on fluid spheres in Finselarian gravity

The motivation behind this article is studying the configurations of compact bodies under the effects of Finselarian gravity in spherical symmetric spacetime coordinates. To examine the effects of gravity on compact stellar configurations, we use the Tolman–Kuchowicz components for spherical symmetric spacetime. We use the linear equation of state to find the function u 0 ′ ( r ) involved in Finselsian gravity. We analyze the configurations using the data for the mass and radius for compact candidates H e r X − 1 , S M C X − 1 , L M C X − 4 , C e n X − 3 . All the star structures that are considered here are stable and ideally free of a central singularity. A detailed graphical investigation reveals that several physical properties, such as density, pressures, sound speeds, TOV forces, mass function, and compactification implemented in celestial formations are critical to their formation. Moreover, we conclude that our stellar models behave well and are acceptable.

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