The purpose of this paper is to investigate the definition of complexity for static anisotropic cylindrical objects in the background of f (G, T ) gravity, where G and T stand for Gauss–Bonnet term and trace of the energy–momentum tensor, respectively. We develop the modified field equations, Tolman–Oppenheimer–Volkoff equation, mass distribution and structure scalars. The complexity is calculated from the splitting of the Riemann tensor in terms of a complexity factor which is associated with the physical characteristics (anisotropic pressure,inhomogeneous energy density) of the system. The zero complexity condition is derived as a constraint to estimate the behaviour of two compact objects corresponding to Gokhroo and Mehra ansatz and polytropic equation of state.We conclude that the addition of f (G, T ) terms contribute to the increment in the complexity of the system.

This paper aims to examine the composition of various spherically symmetric star models which are coupled with anisotropic configuration in f ($R$, $T$, $Q$) gravity, where $Q = R_{\chi}{\xi}T^{\chi}{\xi}$. We discuss the physical features of compact objects by employing bag model equation of state and construct the modified field equationsin terms of Krori–Barua ansatz involving the unknowns (A, B,C). The observational data of 4U 1820-30, Vela X-I, SAX J 1808.4-3658, RXJ 1856-37 and Her X-I are used to calculate these unknowns and bag constant B$_c$.Further, we observe the behaviour of energy density, radial and tangential pressure as well as anisotropy through graphical interpretation for a viable model $R+{\varrho}Q$ of this gravity. For a particular value of the coupling constant ${\varrho}$, we study the behaviour of mass, compactness, red-shift and the energy bounds. The stability of the considered stars is also checked by using two criteria.We conclude that our structure developed in this gravity is in good agreement with all the physical requirements.