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.
Axially symmetric dissipative fluids in the quasi--static approximation
使用一个框架的基础上的$1+3$形式主义，我们进行了研究轴对称和反射对称耗散流体，在准静态制度。我们首先推导出一组不变定义的“速度”，这使得一个明确的定义准静态近似。接下来，我们重写这个近似中的所有相关方程，并提取所有可能的、物理上相关的、遵循这种近似的结果。特别是，我们展示了如何涡，剪切和耗散通量，可能会导致的情况下，不同种类的“速度”的变化的迹象内的流体分布相对于他们的符号在边界表面上。结果表明，引力辐射态与准静态态不是{ \it a priori}不相容的.然而，任何这样的状态都必须持续无限长的时间，从而减少了它的物理相关性。
