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.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have