  Motivated by the increasing evidence for the need of a geometry that
resembles Bianchi morphology to explain the observed anisotropy in the WMAP
data, we have discussed some features of the Bianchi type-$VI_{0}$ universes in
the presence of a fluid that wields an anisotropic equation of state (EoS)
parameter in general relativity. We present two accelerating dark energy (DE)
models with an anisotropic fluid in Bianchi type-$VI_{0}$ space-time. To
prevail the deterministic solution we choose the scale factor $a(t) =
\sqrt{t^{n}e^{t}}$, which yields a time-dependent deceleration parameter (DP),
representing a class of models which generate a transition of the universe from
the early decelerating phase to the recent accelerating phase. Under the
suitable condition, the anisotropic models approach to isotropic scenario. The
EoS for dark energy $\omega$ is found to be time-dependent and its existing
range for derived models is in good agreement with the recent observations of
SNe Ia data (Knop et al. 2003), SNe Ia data with CMBR anisotropy and galaxy
clustering statistics (Tegmark et al. 2004) and latest combination of
cosmological datasets coming from CMB anisotropies, luminosity distances of
high redshift type Ia supernovae and galaxy clustering (Hinshaw et al. 2009;
Komatsu et al. 2009). For different values of $n$, we can generate a class of
physically viable DE models.The cosmological constant $\Lambda$ is found to be
a positive decreasing function of time and it approaches to a small positive
value at late time (i.e. the present epoch) which is corroborated by results
from recent type Ia supernovae observations. We also observe that our solutions
are stable. The physical and geometric aspects of both the models are also
discussed in detail.
