On the other hand, several researchers [15-17] focused on the fact that Wilkinson Microwave Anisotropy Probe (WMAP) data [18, 19] requires Bianchi type morphology instead of Friedman-Robertson-Walker (FRW) type for better accurate explanation of the anisotropic universe.
In the presence of EMT, Einstein's field equations (2) corresponding to Bianchi type V space-time (1) lead to the following:
Kilinc, "LRS Bianchi type I models with anisotropic dark energy and constant deceleration parameter," General Relativity and Gravitation, vol.
Here a > 0 Bianchi type
[alpha] [n.sup.1] [n.sup.2] [n.sup.3] [VII.sub.a] a 0 1 1 [III.sub.a=1] 1 0 1 -1 VI.sub.a [not a 0 1 -1 equal to] 1] [[??].sup.
In Section 2.1 we present the Einstein-Klein-Gordon-like equations in general way and also as an application to the Bianchi type [VI.sub.h=-1] case in terms of the radii of the cosmological model.
Now with expression (4) we proceed to build up the Lagrangian and the Hamiltonian of the theory at the classical regime employing the anisotropic cosmological Bianchi type [VI.sub.h=-1] model.
Since we are interested in anisotropic background, we are going to assume that the four-dimensional metric [g.sub.[alpha][beta]] is described by the Bianchi type [VI.sub.h=-1] model whose line element can be read as (we write in usual way and in Misner's parameterization)
Divya Prasanthi, "Bianchi type VI0 generalized ghost pilgrim dark energy model in Brans-Dicke theory of gravitation," Canadian Journal of Physics, vol.
Amirhashchi, "Probing dark energy in the scope of a Bianchi type I spacetime," Physical Review D, vol.
Bianchi type models are among the simplest models with anisotropic background.
Here we take the spatially homogeneous, anisotropic, LRS Bianchi type I space-time
Now, for LRS Bianchi type I space-time (5), the field equations (2) take the form