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Constraining $f(R)$ Gravity Models with The Late-Time Cosmological Evolution

The $f(R)$ Modified Gravity is a modification of Einstein's general theory of relativity, which aims to explain issues beyond The Standard Model of Cosmology such as dark energy and dark matter. As a theory of gravitation that govern major dynamics on the large scale of the universe, an $ f(R)$ model should be able to explain the transition from a matter-dominated universe to a dark-energy-dominated universe. Assuming that the density parameter of the radiation can be neglected during the transition from a matter-dominated universe to a dark-energy-dominated universe, we find some fixed points regarding the dynamical stability of the density parameters of the model. The phase transition can be achieved if the $f(R)$ model can connect the fixed point $P_5$ (representing the matter-dominated era) to the fixed point $P_1$ (representing the dark energy-dominated era). The method to evaluate that state transition is called the Fixed-point analysis. In this study, we analyze the viability of $f(R)$ models proposed by Starobinsky, Hu-Sawicki, and Gogoi-Goswami regarding the phase transition from a matter-dominated universe to a dark-energy-dominated universe. It is shown that those models are viable by choosing some set of appropriate parameters. For example, in the Starobinsky and Hu-Sawicki models, the parameter $μ$ can be chosen to correspond to the lower bound of $x_d= R_1/Rc$, where $R_1$ represents the de-Sitter point. Meanwhile, for the Gogoi-Guswami model, the same results can be achieved by taking $α$ and $β$ parameters satisfying the existence and stability conditions for the de-Sitter point. From these results, it can be concluded that those $f(R)$ models allow such phase transitions of the universe to realize the late-time accelerated expansion.