Anirudh Pradhan

Bianchi Type-III String Cosmological Models with Time Dependent Bulk Viscosity

Bianchi type-III string cosmological models with bulk viscous fluid for massive string are investigated. To obtain the determinate model of the universe, we assume that the coefficient of bulk viscosity ξ is inversely proportional to the expansion θ in the model and expansion θ in the model is proportional to the shear σ. This leads to B = lCn, where l and n are constants. Behaviour of the model in the presence and absence of bulk viscosity is discussed. The physical implications of the models are also discussed in detail.

BIANCHI TYPE I MAGNETOFLUID COSMOLOGICAL MODELS WITH VARIABLE COSMOLOGICAL CONSTANT REVISITED

The behaviour of magnetic field in anisotropic Bianchi type I cosmological model for bulk viscous distribution is investigated. The distribution consists of an electrically neutral viscous fluid with an infinite electrical conductivity. It is assumed that the component

An Interacting Two-Fluid Scenario for Dark Energy in an FRW Universe

\sigma^1_1

BULK VISCOUS FRW COSMOLOGY IN LYRA GEOMETRY

of shear tensor

Dark energy model in anisotropic Bianchi type-III space-time with variable EoS parameter

\sigma^j_i

Bianchi Type-V Cosmology in f(R,T) Gravity with Λ(T)

is proportional to expansion (θ) and the coefficient of bulk viscosity is assumed to be a power function of mass density. Some physical and geometrical aspects of the models are also discussed in presence and also in absence of the magnetic field.

SOME BIANCHI TYPE I VISCOUS FLUID COSMOLOGICAL MODELS WITH A VARIABLE COSMOLOGICAL CONSTANT

We study the evolution of the dark energy parameter within the scope of a spatially homogeneous and isotropic Friedmann—Robertson—Walker (FRW) model filled with barotropic fluid and dark energy. To obtain the deterministic solution we choose the scale factor , which yields a time-dependent deceleration parameter (DP). In doing so, we consider the case minimally coupled with dark energy to the perfect fluid as well as direct interaction with it.

Some Bianchi Type III String Cosmological Models with Bulk Viscosity

We have studied an isotropic homogeneous FRW universe in the presence of a bulk viscous fluid within the framework of Lyras geometry. We have obtained exact solutions of the Sen equations assuming the deceleration parameter to be constant. The coefficient of bulk viscosity has been assumed to be a power function of the mass density. With this assumption, we have considered the behavior of the displacement field and the energy density for both power-law and exponential expansions of the universe. We show that our models are generalised and we obtain the results of previous works by considering k=0 and k=-1.

Two-fluid scenario for dark energy models in an FRW universe-revisited

A new dark energy model in anisotropic Bianchi type-III space-time with variable equation of state (EoS) parameter has been investigated in the present paper. To get the deterministic model, we consider that the expansion θ in the model is proportional to the eigen value

Bianchi Type-I Massive String Magnetized Barotropic Perfect Fluid Cosmological Model in General Relativity

\sigma^{2}_{~2}