Dissipative Unified Dark Fluid Model
  We consider a unified dissipative dark fluid model. Our fluid contains an
adiabatic part plus a bulk viscous one. The adiabatic part has the ability to
asymptote between two power laws and so can interpolate between the dust and
dark energy equations of state at early and late times. The dissipative part is
a bulk viscous part with constant viscosity coefficient. The model is analyzed
using the phase space methodology which helps to understand the dynamical
behavior of the model in a robust manner without reference to the system
solution. The parameters of the model are constrained through its asymptotic
behavior and also through many observational constraints. We solve the Hubble
parameter equation using numerical methods and results are plotted against the
newest set of Hubble data. The model is tested using the $Om(z)$ test which
shows that this model although is a quintessence-like model, it slides through
the phantom barrier. We study the model expectations for the evolution of the
universe by studying the evolution of the deceleration parameter, the density
of the universe, the effective equation of state parameter of the model and of
its underlying dark energy package. We estimate the value of the present day
viscosity coefficient of the cosmic fluid as $8 \times 10^6 Pa.s$, which agrees
with the work of many authors, e.g., Velten and Schwartz [26], Wang and Meng
[27], and Sasidharan and Mathew [29]. We argue that this model is able to
explain the behavior of the universe evolution.
