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We have provided a new exact solution for anisotropic compact stars to the field equations of f(R,T)-gravity via a decoupling technique, with the assumption of a linear f(T)function and the modified Durgapal-Fuloria metric ansatz. By deforming the radial component of the metric and introducing Pseudo-Isothermal (PI) dark matter (DM) as a new source to the anisotropic seed solution in the process of minimally gravitational decoupling, we have obtained a non-singular solution that meets all physical criteria related to effective density, effective pressure, effective anisotropy, and energy conditions. The present system satisfies the modified Tolman-Oppenheimer-Volkoff equation and achieves stable equilibrium, fulfilling stability criteria such as the adiabatic condition, Herrera cracking concept, and Harrison-Zeldovich-Novikov condition. The influence of minimally gravitational decoupling on the characteristics of the system has been illustrated graphically by varying the decoupling constant (γ). The mass-radius relations are linked to observational constraints and examined for anisotropic stellar systems with and without the effect of minimally gravitational decoupling in both general relativity (GR) and f(R,T)-gravity. We found that increasing values of the f(R,T)-gravity parameter (χ) and γreduce the maximum allowable mass of the star. Therefore, increasing the effects of minimally gravitational decoupling and the PI-DM content, subject to the Durgapal-Fuloria metric potential ansatz, cannot support highly compact and supermassive astrophysical objects.

This study delves into the distinctive characteristics of wormhole models in the context of de Rham-Gabadadze-Tolley (dRGT) massive gravity, providing insights into their theoretical behavior and stability. We use a null zero complexity factor to find the wormhole shape function for Model I. Additionally, we solve analytically the modified field equations describing wormhole for a given choice of logarithmic redshift function, exploiting the Karmarkar condition for embedding class one metrics for Model II. To achieve this, we analyze the wormhole geometry in a static spherical spacetime with an anisotropic matter configuration. The study investigates a number of parameters, including density, energy conditions, equation of state parameter, adiabatic sound velocity, and equilibrium condition. The solution shows a traversable wormhole that violates the null energy criterion and equilibrium state for certain ranges of free parameters. We employ adiabatic sound velocity analysis to concentrate on the stability of the wormhole. Furthermore, by using the equation of state parameter (ω), we conclude that both models end up in the phantom dark energy region. Finally, our findings highlight distinct photon deflection behaviors in dRTG massive gravity, with Model II showing negative angles indicative of repulsive gravity, while Model I exhibits positive angles, underscoring significant differences in gravitational dynamics.

In the present paper, we have explored the existence of compact structures describing anisotropic matter distributions within the framework of f(R,T)theory, where Ris Ricci scalar and Tis a trace of energy–momentum tensor. We have chosen f(R,T)as a linear function of Rand T, i.e., f(R,T)=R+2χTwith χas matter-geometry coupling constant. We employed the embedding class one technique in order to obtain a full space–time description inside the stellar configuration. After specifying space–time geometry, we determined the complete solution of modified field equations by using the MIT-Bag model equation of state, i.e., pr=13(ρ−4Bg)that describes the strange quark matter distribution inside the stellar system, where Bgrepresents a bag constant. We checked the physical viability of the solution through different physical tests. Moreover, using observed mass values for the various strange star candidates, we have predicted the exact radii by taking distinct values for χand Bg. Accordingly, we thoroughly show that with decreasing the value of χ, the stellar systems under examinations become progressively massive and larger in size, transforming them into less dense compact objects. It additionally uncovers that for χ<0the fR,Tgravity arises as an adequate theory for explaining the magnetars, super-Chandrasekhar stars and massive pulsars, which are assumed to be the reason behind the overluminous SNeIa e.g. SN 2003fg, SN 2006gz, SN 2007if, SN 2009dc and remain mostly unexplained in the background of general relativity.