Abstract： The Bianchi type-III cosmological model for a cloud string with bulk viscosity are studied. To obtain a determinate solution, it is assumed that the coefficient of bulk viscosity is a power function of the
scalar of expansion zeta = kθm and the shear scalar is proportional to scalar of expansion σ ∝ θ, which leads to the relation between metric potentials B = Cn. The physical features of the model are also discussed. It is found that the power index m has significant influence on the string model. There is a ``big bang'' start in the model when m≤1 but there is no the big-bang start when m > 1. In the special case m = 0, the model reduces to the string model of constant coefficient of bulk viscosity that was the result previously given in the literature.
(Particle-theory and field-theory models of the early Universe (including cosmic pancakes, cosmic strings, chaotic phenomena, inflationary universe, etc.))
引用本文:
WANG Xing-Xiang. Bianchi Type-III String Cosmological Model with Bulk Viscosity in General Relativity[J]. 中国物理快报, 2005, 22(1): 29-32.
WANG Xing-Xiang. Bianchi Type-III String Cosmological Model with Bulk Viscosity in General Relativity. Chin. Phys. Lett., 2005, 22(1): 29-32.
2005, Vol. 22 
