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Common phenomenological parametrizations of the equation of state parameter are the Chevallier-Polarski-Linder parametrization [70 71 baldi ] :  \begin{equation} w(a) = w_0 + w_a (1-a) \end{equation}  based on the behavior of w(a) at low redshifts, and the early dark energy parametrization [ look at fontanot ]   \begin{equation} w(a) = \frac{w_0}{1+b ln(1/a)}\end{equation} \text{ln}(1/a)}\end{equation}  where $b$ is a parameter dependant on the the abundance of Dark Energy at early times. times.\\  Another class of widely studied scenarios views dark energy Dark Energy  as a scalar field whose dynamical evolution is driven by a parametrized potential, the representative models of this class are Quintessence [b], k-essence[b], Phantom[b], Quintom [b] and perfect fluid [] DE models.For Dark Energy models. For  Quintessence models the most common choices of potentials include slowly varying runaway potentials such as an inverse power law [ b]: \begin{equation}equation\end{equation} \begin{equation} V(\phi) = A \phi^{-\alpha} \end{equation}  or an exponential [b]:  \begin{equation}equation\end{equation} \begin{equation} V(\phi) = A e^{-\alpha \phi} \end{equation}  or SUGRA potentials arising within supersymmetric theories of gravity [b] :  \begin{equation}equation\end{equation}  in k-essence models instead the it’s the scalar field kinetic energy that drives the acceleration.