Abstract
Magnetized Anti-stiff fluid Cosmological Models with Variable Cosmological Constant
Highlights
Recent theoretical cosmological observations [1] suggested that the expansion of the universe is accelerating
Bianchi type-III model ( m 1): FRW models are homogeneous and isotropic. These isotropic models are unstable near the origin and fail to describe the early universe [46], but anisotropy plays a significant role in the models near t = 0, spatially homogeneous and anisotropic Bianchi type models are undertaken to study the universe at its early stage of evolution
We have studied Bianchi type-III and Kantowski Sachs cosmological model containing perfect fluid with magnetic field in general theory of relativity
Summary
Recent theoretical cosmological observations [1] suggested that the expansion of the universe is accelerating. In Einstein’s general relativity, in order to have such acceleration, one needs to introduce a component to the matter distribution of the universe with a large negative pressure. This component is usually referred as Dark Energy (DE). Recent observations indicate that 10 55cm 2 while the particle physics prediction for is greater than this value by a factor of order 10120 This discrepancy is known as the cosmological constant problem. The study of magnetic field in the matter distribution is of considerable interest as it provides an effective way to understand the initial phases of cosmic evolution. Banerjee et al [21] have investigated an axially symmetric Bianchi Type I
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