increasing $t$, reflecting that the Early Universe was likely expanding. Also the life time of the thermal viscous Universe seems to be shorter than for the non-viscous Universe. Almost the same behavior is observed in the right panel of Fig. \[Figg2\]. The temperature $T$ seems to be finite at vanishing $t$ in the viscous Universe. The $T$-singularity is only present, if we assume that the background matter is non-viscous ideal gas.

In left panel of Fig. \[Figg3\], we show the dependence of the bulk viscous pressure $\Pi$ on $t$. $\Pi$ takes negative values at very small $t$. Then it switches to positive values at some values of $t$. After reaching the maximum value, $\Pi$ decays exponentially with increasing $t$. At larger $t$, $\Pi$ entirely vanishes. The deceleration parameter $q$, given by Eq. (\[approx-q\]), is depicted in the right panel of Fig. \[Figg3\], and it is compared with $q$ for a non-viscous fluid, $q=-3$. The approximate solution, given by Eq. (\[approx-q\]), results in negative $q$ at small $t$, referring to expansion era. $q$ from the particular solution, Eq. (\[partcq\]) is negative everywhere.\
For the particular solution, only the scale factor depends on $t$, Eq. (\[partca\]). The results are given in the 