Abstract
This study investigates models of a non-singular cosmic bounce for the Friedmann-Robertson-Walker spacetime in the framework of f(ℚ) gravity (ℚ represents the non-metricity scalar). Our derivations lead to the modified field equations whose solutions are subsequently analyzed across a range of parameter values. To understand how this gravitational model influences cosmic history, we examine specific algebraic polynomial and exponential forms of f(ℚ). We then study key cosmological parameters to identify conditions that allow viable bounce solutions. It is found that energy density is positive and pressure is negative, while the energy conditions are violated, which are instrumental in achieving a coherent cosmological bounce. We can conclude that this gravitational theory provides a compelling substitute to establish cosmological frameworks, leading to the understanding of the universe initial phases.