an effective equation of state $\gamma_{eff}=2$;

which allows us to conclude that the introduction of $F$ in the Friedmann universe has the role to encode all the viscous effects in the dynamics and what we see at the end is the usual ideal fluid equation of state. We say in this sense that bulk viscosity is regularized.\
Now we emphasize that by extrapolating our solutions to the regime $\beta_{2}>\nicefrac{1}{2}$ we obtain an intriguing dynamical property of the Universe. In fact, from equation (\[gammaeff\]) for $\beta_{2}=1/2+\varepsilon$ with $\varepsilon>0$ we immediately get $$\gamma_{eff}=\frac{1}{1+\varepsilon}\rightarrow p=-\frac{\varepsilon}{(1+\varepsilon)}\rho.$$ For $\varepsilon>\nicefrac{1}{2}$ (i.e. $\beta_{2}>1$ and $\gamma_{eff}<\nicefrac{2}{3}$) this dynamical behavior corresponds to a powerlaw inflation solution, induced by a negative effective pressure $p<-\nicefrac{1}{3}\rho$. Indeed, it is easy to realize that the cosmological horizon $$d_h(t)\equiv R(t) \int_{0}^{t}\frac{dt'}{R(t')}$$ takes in this case a divergent value. In this scenario the Universe corresponds to a unique causal region and we can think of it as a viable solution to the horizon paradox. It is worth noting that, since we are dealing with an isotropic flat Universe, we get $H\sim \sqrt{\rho}$ (see equation (\[integrale3\])). Then, the restriction $\beta_{2}< \nicefrac{1}{2}$ in the expression (\[visc2\]), derived for an Eckart representation of the fluid ($F\equiv 1$), acquires 