  We study a cosmology by considering entropic issues. We make a bare/effective
description of the equation of state of the cosmic fluid through a bare
(\omega)/effective (\omega_eff) conservation equation. In the bare case, where
we have a non conserved equation of state for the cosmic fluid, we describe the
change in the sign of the inhomogeneus term at different times of the cosmic
evolution. We show that by a redefinition of the adiabatic \omega -parameter we
can recover the usual scheme for the cosmic evolution. In the effective case we
show also that if the evolution is driven by dust or cosmological constant, the
universe evolves on the thermal equilibrium. Additionally, by incorporating a
quantum correction only cosmological constant can drive an evolution on thermal
equilibrium.
