Speaker
Description
In the present work, we have constructed an anisotropic dark energy cosmological model in the framework of General Relativity at the backdrop of spatially homogeneous and anisotropic Bianchi V metric. The anisotropic behaviour of the model is simulated through the consideration of different scale factors and Hubble expansion rates along different spatial directions. A parameter $m$ is considered to take care of the anisotropic behaviour of the model in the sense that, if $m=1$, we get isotropic model and for $m\neq 1$, anisotropic nature will be retained. The cosmic fluid is also considered to be anisotropic which allow us to assume different pressure of the fluid along different directions.
Summary
Anisotropic dark energy model with dynamic pressure anisotropies along different spatial directions is constructed at the backdrop of a spatially homogeneous diagonal Bianchi type $V$ $(BV)$ space-time in the framework of General Relativity. A time varying deceleration parameter generating a hybrid scale factor is considered to simulate a cosmic transition from early deceleration to late time acceleration. We found that the pressure anisotropies along the $y-$ and $z-$ axes evolve dynamically and continue along with the cosmic expansion without being subsided even at late times. The anisotropic pressure along the $x-$axis becomes equal to the mean fluid pressure. At a late phase of cosmic evolution, the model enters into a phantom region. From a state finder diagnosis, it is found that the model overlaps with $\Lambda$CDM at late phase of cosmic time.
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