Abstract
This paper aims to explore some realistic configurations of anisotropic spherical structures in the background of metric f(R) gravity, where R is the Ricci scalar. The solutions obtained by Krori and Barua are used to examine the nature of particular compact stars with three different modified gravity models. The behavior of material variables is analyzed through plots and the physical viability of compact stars is investigated through energy conditions. We also discuss the behavior of different forces, equation of state parameter, measure of anisotropy and Tolman–Oppenheimer–Volkoff equation in the modeling of stellar structures. The comparison from our graphical representations may provide evidence for the realistic and viable f(R) gravity models at both theoretical and the astrophysical scale.
Highlights
The modified theories of gravity are generalized models; they came into being by modifying only the gravitational portion of the General relativity (GR) action
In f (R) gravity, the NEC and WEC are formulated as NEC ⇔ ρeff + pieff ≥ 0, WEC ⇔ ρeff ≥ 0 and ρeff + pieff ≥ 0, while the SEC and the dominant energy condition (DEC) yield
This paper is devoted to a discussion of some physical aspects of spherically symmetric compact stars in the background of metric f (R) theory
Summary
The modified theories of gravity are generalized models; they came into being by modifying only the gravitational portion of the GR action (for further reviews on DE and modified gravity, see, for instance, [8,9,10,11,12,13,14,15,16,17,18,19,20,21,22]). Santos et al [72] developed viability bounds coming from ECs on a generic f (R) formalism Their approach could be considered to constrain various possible f (R) gravity models with proper physical backgrounds. In order to achieve some realistic results for the modeling of an anisotropic compact stellar structure, we use a specific combination of metric variables, i.e., a(r ) = Br 2 + C and b(r ) = Ar 2, as suggested by Krori and Barua [85]. The evolution of stellar structure could end up with white dwarfs, neutron stars or black holes, depending upon their initial mass configurations. In order to investigate the equilibrium conditions, we shall study the impact of hydrostatic, gravitational and anisotropic forces, in the possible modeling of compact stars
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