In the present paper, we have investigated Bianchi type II, VIII and IX spacetime in the presence of magnetized anisotropic dark energy in the Scale covariant theory of gravitation. Exact solution of the field equations are obtained by assuming the expansion anisotropy (the ratio of shear scalar to expansion scalar) to be a function of average scale factor. The isotropy of the fluid, space and expansion are examined.

We consider a self-consistent system of Plane symmetric cosmology and binary mixture of perfect fluid and dark energy. The perfect fluid is taken to be one obeying the usual equation of state p = γρ with γ ∈ [0, 1]. The dark energy is considered to be either the quintessence or Chaplygin gas. Exact solutions to the corresponding Einstein's field equations are obtained as a quadrature. The cases of Zeldovich Universe, Dust Universe and Radiation Universe and models with power-law and exponential expansion have discussed in detail. For large t, the models tend to be isotropic.

We study the spatially homogeneous Kaluza-Klein cosmological model with magnetized anisotropic fluid in the scalar tensor theory of gravitation proposed by Brans-Dicke [1]. Exact solutions of the models are obtained by Volumetric exponential and power law expansion. The Physical behaviors of the models have been discussed using some physical quantities.

The paper deals with an anisotropic Bianchi type VI o cosmological model with variable ω in the presence and absence of magnetic field of energy density ρ B . A special law of variation for Hubble's parameter proposed by Berman (Nuovo Cimento B 74:182, 1983) has been utilized to solve the field equations.

Kantowski-Sachs cosmological model in the presence of magnetized anisotropic dark energy is investigated. The energy-momentum tensor consists of anisotropic fluid with anisotropic EoS p = ωρ and a uniform magnetic field of energy density ρ B . We obtain exact solutions to the field equations using the condition that expansion is proportional to the shear scalar. The physical behavior of the model is discussed with and without magnetic field. We conclude that universe model as well as anisotropic fluid does not approach isotropy through the evolution of the universe.