Dark Energy Universe in Bianchi Type-I Cosmological Model
In the present work, there is a trend to modify the earlier models (supporting the constant rate of expansion), by assuming the time-dependent average scale factor a(t) = [(c1t + c2)(m + 2)]1/3 . Here, we have also revisited the investigation of new holographic dark energy. The Saez-Ballester field equations are solved under certain assumptions and found a power law of expansion. Our model and its current range for DE, ω (EoS) parameter is observed to be in great concurrence from the observations. Also, for the model, Some physical and geometric aspects of the DE model are also highlighted.