Revise the Dark Matter-Phantom Scalar Field Interaction

The cosmological history and evolution are examined for gravitational models with interaction in the dark sector of the universe. In particular, we consider the dark energy to be described by a phantom scalar field and the dark matter \(\rho _{m}\) as a pressureless ideal gas. We introduce the interacting function \(Q=\beta \left( t\right) \rho_{m}\), where the function \(% \beta \left( t\right) \) is considered to be proportional to \(\dot{\phi}, \dot{\phi}^{2}H^{-1},~H\), or a constant parameter with dimensions of \(\left[H_{0}\right] \). For the four interacting models, we study in details the phase space by calculating the stationary points. The latter are applied to reconstruct the cosmological evolution. Compactified variables are essential to understand the complete picture of the phase space and to conclude about the cosmological viability of these interacting models. The detailed analysis is performed for the exponential potential \(V\left( \phi \right) =V_{0}e^{\lambda \phi }\). The effects of other scalar field potential functions on the cosmological dynamics are examined.