Abstract
We investigate some locally rotationally symmetric (LRS) Bianchi type-III string cosmological model in the presence of bulk viscosity and magnetic field, where an equation of state and relation between metric potential are considered. The solution describes a shearing and non-rotating model with big-bang start. In the absence of magnetic field it reduces to a string model with bulk viscosity, where the relation between the coefficient of bulk viscosity and the energy density is for a = 0.
Highlights
It is a challenging problem to determine the exact physical situation at the early stages of formation of our universe
In the absence of magnetic field it reduces to a string model with bulk viscosity, where the relation between the coefficient of bulk viscosity and the energy density is 2 for α = 0
Tikekar and Patel [8] and Chakraborty and Chakraborty [9] have presented the exact solutions of Bianchi type III and spherically cosmology respectively for a cloud string
Summary
It is a challenging problem to determine the exact physical situation at the early stages of formation of our universe. The general relativistic treatment of strings was initiated by Letelier [4] and Satchel [5] This model has been used as source for Bianchi Type I and Kantowski-Sachs cosmologies by Letelier [4]. It is well known that when neutrino decoupling occurs, the matter behaves as a viscous fluid in an early stage of the universe. Viscous fluid cosmological model of early universe have been widely discussed in the literatures [10,11]. Bali et al [19] has studied Bianchi type VIo magnetized bulk viscous massive string cosmological model in general relativity. We study string cosmology with bulk viscosity and magnetic fluid for Bianchi type III.
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