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 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. 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, 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 10 VI. RESULTS H ( t ) = 1 2 t , (45) a ( t ) = √$_{t.}$ (46) a ( t ) = a$_{0}$ ( exp( b$_{2}$t ) − b$_{1}$ exp( b$_{2}$t ) ) 1 /b$_{1}$ , (40) ρ ( t ) = 3 b$_{2}$ exp( − b$_{2}$t 1 − b$_{1}$ exp( − b$_{2}$t ) ) 2 , (41) T ( t ) = 3 r β ( b$_{2}$ exp( b$_{2}$t 1 − b$_{1}$ exp( − b$_{2}$t ) ) , (42) Π( t ) = b 2 $_{2}$[2 exp( b$_{2}$t ) − 3 γ ] [exp( b$_{2}$t ) − b$_{1}$ ] 2 , (43) q ( t ) = exp( b$_{2}$t ) − 1 . (44)