Exploring Physical Properties of Gravitationally Decoupled Anisotropic Solution in 5D Einstein‐Gauss‐Bonnet Gravity

Abstract

In this paper we present two new classes of solutions describing compact objects within the framework of five‐dimensional Einstein‐Gauss‐Bonnet (EGB) gravity. We employ the Complete Geometric Deformation (CGD) formalism which extends the Minimal Geometric Deformation (MGD) technique adopted in earlier investigations to generate anisotropic models from known isotropic solutions. The two solutions presented arise from mimicking the constraint for the pressure and density respectively which generate independent deformation functions. Rigorous physical tests show that contributions from CDG suppress the effective pressure but enhances the effective density and mass of the compact object, with the suppression/enhancement being modified by the EGB coupling constant. One of the highlights in our findings is that the deformation function along the radial component in CDG is nonzero at the boundary when we mimic both the pressure and density while in MGD we observe a vanishing of this deformation function at the boundary of the fluid configuration only for the pressure constraint. The difference in behavior of the deformation function at the surface predicts different stellar characteristics such as mass‐to‐radius and surface redshifts.

An anisotropic extension of Heintzmann IIa solution with vanishing complexity factor

“…[32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48][49]). Even this framework has been used widely in several scenarios such as 2 + 1 space-times [50][51][52][53][54][55], higher dimensions [56,57], asymptotically (A-)dS space-times [58], for axially symmetric systems and rotating black holes [59], hairy black holes [60][61][62], Cosmology [63,64], solutions in the background of Reissner-Nordström space-time [65][66][67], modified gravity theories [68][69][70][71][72][73][74][75][76][77][78], as well in braneworld gravity [79][80]…”

Gravitationally decoupled anisotropic solution using polytropic EoS in the framework of 5D Einstein–Gauss–Bonnet Gravity

“…We now only need to solve the second system corresponding to θ -sector which depends on the undetermined deformation function ψ(r ), in order to find the complete solution for energy-momentum tensor T eff μν . In GR, a wide variety of approaches have been adopted to obtain the deformation function, ψ(r ) [24,[29][30][31] but very few in the context of 5D EGB gravity [26][27][28]. In this work we mimic the seed energy density (r ) to θ 0 0 (r ) i.e.…”

“…Then, it may not be possible to embed the stellar compact object to vacuum space-time. But, if we assume that new contributions arising from θ μν are confined within the stellar interior [24,28], then the stellar compact object will remain embedded into a true Boulware-Deser vacuum space-time (52). Now we the fix easily the arbitrary constant parameters by joining of the interior (51) and exterior (52) spacetimes across the boundary.…”

“…Recent work on EGB stars via the MGD technique has shown that it is possible to obtain stable neutron star models [26] as well as beyond the conventionally observed upper limit of two solar masses [27]. In addition, a first detailed study of the CGD approach in 5D EGB gravity is also discovered by Maurya et al [28]. Some of the rigorous works in different contexts except 5D gravity under gravitational decoupling via MGD approach and its extension can be found in the following works .…”

Anisotropic Strange Star Model Beyond Standard Maximum Mass Limit by Gravitational Decoupling in f(Q)$f(Q)$ Gravity

“…Some of the recent research results in GR, f (R, T) and f (G) gravity theories can be seen in the references. [44][45][46][47][48][49][50][51][52][53][54] In this connection, the first systematic approach for MGD and extended MGD in 5D EGB gravity was proposed by Maurya et al [55,56] to obtain the exact solution of the compact star model. Recently, Maurya et al [57] have shown the impact of the decoupling parameter and the EGB constant on the maximum mass limit on minimally deformed neutron star models.…”