Some Exact Solutions of Magnetized viscous model in String Cosmology

TL;DR

This paper derives exact solutions for anisotropic magnetized viscous string cosmological models, analyzing their effects on universe evolution and the role of bulk viscosity and magnetic fields in different string scenarios.

Contribution

It introduces new exact solutions for magnetized viscous string cosmology models, exploring their physical implications in early and late universe stages.

Findings

Bulk viscosity influences universe density evolution.

Magnetic fields affect classical potential and density parameters.

Bulk viscosity prevents the universe from becoming empty in the future.

Abstract

In this paper, we study anisotropic Bianchi-V universe with magnetic field and bulk viscous fluid in string cosmology. Exact solutions of the field equations are obtained by using the equation of state for a cloud of strings, and a relationship between bulk viscous coefficient and scalar expansion. The bulk viscous coefficient is assumed to be inversely proportional to the expansion scalar. It is interesting to examine the effects of magnetized bulk viscous string model in early and late stages of the evolution of the universe. This paper presents the different string models like geometrical (Nambu string), Takabayashi (p-string) and Reddy string models by taking certain physical conditions. We discuss the nature of the classical potential for viscous fluid with and without magnetic field. We find that the introduction of bulk viscosity with and without magnetic field results in rapid change in density parameters and in the classical potential. The presence of bulk viscosity prevents the universe to be empty in its future evolution. The other physical and geometrical aspects of each string model are discussed in detail.