In this study, we investigate the attributes of compact stars within the configuration of f ( G , φ ) gravity, by incorporating the Gauss-Bonnet term G and a scalar field φ. By adopting different functional forms of f ( G , φ ) , we analyze their impact on the equilibrium structure of dense stellar objects. Further, we adopt the Krori-Barua metric potential, defined as ν ( r ) = B r 2 + C and λ ( r ) = A r 2 , here, A, B and C are constants. To ensure a physically viable compact configuration, we impose matching conditions between the interior spherically symmetric space-time and the Schwarzschild geometry. Moreover, we investigate the attributes of the celestial star models by assuming the f ( G , φ ) gravity model. We attain the modified field equations and examine key physical characteristics, namely energy density and pressure components, stability conditions, equation of state, and energy constraints. These findings provide new insights into the viability of alternative gravity models in explaining extreme astrophysical environments and offer potential observational signatures to constrain f ( G , φ ) gravity through future gravitational wave and electromagnetic observations.
Asghar et al. (2026) studied this question.