  In this paper, we have assumed a flat Friedmann-Lemaitr\'e-Robertson-Walker
universe endowed with a general form of dissipation. The source of dissipation
is considered to be a bulk viscous pressure $\Pi$ which leads to an adiabatic
creation of particles induced by the gravitational field. Further, the cosmic
substratum is assumed to satisfy the equation of state $p=(\gamma -1)\rho$ and
$\Pi$ is considered to be proportional to $H^{2k+1}$, where $H$ is the Hubble
parameter and $k$ is the index of dissipation. This choice of dissipation is
consistent with the pioneering works by Barrow and Clifton. Finally, by
assuming an exponential form for $H$ given by $H=e^{m(t-t_0)}$, where $m$ is a
positive real parameter and which bears all the signatures of an emergent
universe, we have been able to establish that the sufficiency of the inequality
$\gamma k \leq 0$ can produce a class of emergent universes. However, this
condition is by no means necessary for the existence of an emergent universe.
