content_image/367726.jpg content_image/367727.jpg content_image/367728.jpg content_image/367729.jpg content_image/367730.jpg content_image/367724.jpg content_image/367725.jpg
where minus sign in the exponential function refers to flipping the integral limits. This was not necessary while deriving the expressions given in Section III. The free parameter P compensates it. The geometric and thermodynamic quantities of the Universe read 

<img src='content_image/367726.jpg'>

<img src='content_image/367727.jpg'>

<img src='content_image/367728.jpg'>

<img src='content_image/367729.jpg'>

<img src='content_image/367730.jpg'>

Obviously , we notice that the scale parameter in Eq. (40) looks like Eq. (24), which strongly depends on the free parameter P . The other geometric and thermodynamic quantities find similarities in Eq. (25) - (28), respectively. Deceleration parameter q seems to be positive everywhere. 

## VI. RESULTS 

In present work, we have considered the evolution of a full causal bulk viscous flat, isotropic and homogeneous Universe with bulk viscosity parameters and equation of state taken from recent lattice QCD data and heavy-ion collisions. Three classes of solutions of the evolution equation have been obtained. 

In Fig. 1, H ( t ) and a ( t ) are depicted in dependence on the comoving time t . We compare H ( t ), given by Eq. (22), and a ( t ), given by Eq. (24), with the counterpart parameters obtained in the case when the background matter is assumed to be an ideal and non-viscous fluid, described by the equations of state of the non-interacting ideal gas, 

<img src='content_image/367724.jpg'>

<img src='content_image/367725.jpg'>

In the left panel of Fig. 1, H ( t ) = ˙ a/a has an exponential decay, whereas in the non- viscous case, H ( t ) is decreasing according to Eq. (45). The latter is much slower than the former, reflecting the nature of the exponential and linear dependencies. The other 

