In this article we obtain a new anisotropic solution for Einstein’s field equations of embedding class one metric. The solution represents realistic

We presented a non-singular solution of Einstein’s field equations using gravitational decoupling by means of complete geometric deformation (CGD) in the anisotropic domain for compact star models. In this approach both the gravitational potentials are deformed as $$ \nu =\xi +\beta \,h(r)$$ν=ξ+βh(r) and $$ e^{-\lambda }=\mu +\beta \,f(r)$$e-λ=μ+βf(r) , where $$\beta $$β is a coupling constant. Then we solve more complex field equations under above transformations by using a particular form of deformation function h(r) for two different cases namely the mimic constraint for the pressure $$\{p(r)=\theta ^1_1\}$${p(r)=θ11} and the mimic constraint for the density $$\{\rho (r)=\theta _0^0\}$${ρ(r)=θ00} (Ovalle in Phys Lett B 788:213, 2019). The compact star models have been constructed by taking $$M_0/R=0.2$$M0/R=0.2 for two different non-zero values of $$\beta $$β . Moreover, the boundary conditions are also performed for the said complete geometric deformation in the presence of anisotropic matter distribution. We also find pressure, density, anisotropy and causality conditions that are physically acceptable throughout the model. The $$M-R$$M-R curve is also presented to support our model for describing a realistic compact object such as neutron stars.

This research article examines the impact of $$f({\mathcal {Q}},{\mathcal {T}})$$f ( Q , T ) theory on the geometry of charged neutron stars filled with anisotropic matter configuration. Here, $${\mathcal {Q}}$$Q represents non-metricity and $${\mathcal {T}}$$T denotes the trace of energy-momentum tensor. We use a particular functional form of this modified theory to reduce the system’s complexity and derive explicit relations of the energy density and pressure components. Further, we consider viable non-singular solutions to analyze the internal structure of the charged neutron stars. The unspecified parameters in the metric coefficients are evaluated through Darmois junction conditions, which ensures consistency between interior and exterior solutions of the stellar objects. These parameters are then used to explore different physical characteristics such as the behavior of energy density, pressure components, anisotropy, energy bounds, equation of state parameter, compactness and redshift function in the interior of charged neutron stars. The stability and equilibrium states of the charged stellar objects are discussed using the Tolman–Oppenheimer–Volkoff equation and the speed of sound, respectively. Our results suggest that the charged neutron stars are viable and stable in the presence of dark source terms.

The focus of this work is centered on determining whether traversable wormholes admitting Einasto density profile exist within the framework of f(R, T) gravity. Using the Morris–Thorne spacetime, we express the wormhole configuration and formulate the anisotropic gravitational equations for a particular linear modified model. Afterwards, by considering two different (constant and variable) redshift functions, we derive the shape function for wormholes and examine its potential stability. The developed functions conform to the necessary conditions and form a connection between two spacetime regions that are asymptotically flat. We also examine the viability of resulting wormhole solutions by verifying their violation with the null energy conditions. We also investigate the active gravitational mass and the complexity factor for our solutions. The later quantity is found to be negative near the wormhole throat and becomes zero when moving away from this point. Further, various methods of stability analysis are utilized to assess the developed models. Our results suggest that the constructed wormhole geometries meet the necessary conditions, thereby existing within the considered modified gravity.

In this work, we study the role of the vanishing complexity factor in generating self-gravitating compact objects under gravitational decoupling technique in f(Q)-gravity theory. To tackle the problem, the gravitationally decoupled action for modified f(Q) gravity has been adopted in the form $${\mathscr {S}}={{\mathscr {S}}_{Q}}+{{\mathscr {S}}^{*}_{\theta }}$$S = S Q + S θ ∗ , where $${\mathscr {S}}_Q$$S Q denotes the Lagrangian density of the fields which appears in the f(Q) theory while $${\mathscr {S}}^{*}_{\theta } (=\alpha {\mathscr {S}}_{\theta }$$S θ ∗ ( = α S θ , where $$\alpha $$α is just a coupling parameter which controls the deformation) describes the Lagrangian density for a new kind of gravitational sector which has not been included in f(Q) gravity. After that, we developed an important relation between gravitational potentials via a systematic approach (Contreras and Stuchlik in Eur Phys J C 82:706, 2022) using the vanishing complexity factor condition in the context of f(Q) theory. We have used the Buchdahl model along with the mimic-to-density constraints approach for generating the complexity-free anisotropic solution. The qualitative physical analysis has been done along with the mass-radius relation for different compact objects via $$M-R$$M - R curves to validate our solution. It is noticed that the coupling constant $$\beta _1$$β 1 has a definite impact on constraining the mass and radii of the object that are shown in $$M-R$$M - R curves. The obtained results show that the compactness of the objects can be controlled by the coupling parameters.