of the standard cosmological model, namely the horizon and entropy ones. Further remarks should now be done about the obtained solutions (\[Htimepower\]), (\[rho4\]), (\[gammaeff\]) and (\[F\_t\]). Despite the power-law approach given by (\[timepowers\]) is able to provide a satisfactory characterization of the asymptotic behavior of the model under consideration, the underlying cosmological relevance which comes with it leads us to support the solutions with an additional numerical investigation. In this regard, we show in the right panel of figure (1) how the power-law approximation is largely predictive near enough to the singularity, while discrepancies take over as the Universe volume expands. On the other hand, one expects that far from the singularity we assist to a gradual decrease of the role of the viscosity. In figure (1) (left panel) it is shown that the numerical solution for large times tends to overlap the standard inviscid flat Robertson-Walker dynamics. The cosmological picture coming out is consistent with the paradigm of an Universe characterized by a viscous non-equilibrium dynamics close to the Big-Bang whose viscous features are suppressed as the volume expands, recovering the isentropic homogeneous and isotropic Universe (as a consequence of the decreasing value of the energy density).

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