Homogeneous viscous universes with magnetic field II. Bianchi type I spaces

Dynamical systems approach to a Bianchi type I viscous magnetohydrodynamic model

“…Then, R 1 ¼ R 2 ¼ R 3 ¼ 0, and according to Eqs. (17), (20), (22), and (23), the evolution equations (14) become…”

“…Benton and Tupper [16] studied Bianchi type I models with a ''powers-of-t'' metric under the influence of a viscous fluid with a magnetic field. Salvati, Schelling, and van Leeuwen [17] numerically analyzed the evolution of the Bianchi type I universe with a viscous fluid and large-scale magnetic field. Ribeiro and Sanyal [18] studied a Bianchi type VI 0 viscous fluid cosmology with an axial magnetic field in which they obtained exact solutions to the Einstein field equations assuming linear relations among the square root of matter density and the shear and expansion scalars.…”

A Bianchi type II cosmological model of Petrov type D representing an imperfect fluid with a source-free magnetic field

“…Cosmological models with an incident magnetic field of various Bianchi types have been obtained by several authors, e.g. Zeldovich [4], Doroshkevich [5], Jacobs [6], Collins [7], Tupper [8], Roy and Prakash [9], Damiao Soares [10], Tsoubelis [11], Dunn and Tupper [12], Lorenz [13][14][15][16][17], Spokoiny [18,19], Batakis [20], Roy et al [21], Van Leeuwen [22], Salvati et al [23], Banerjee and Sanyal [24], Ribeiro and Sanyal [25], Nayak and Bhuyan [26] and Raychoudhuri [27].…”

Inhomogeneous and anisotropic cosmologies

“…One is that the matter content is generally assumed to be a perfect fluid, although this is strictly incompatible with the other assumed physical properties. Attempting to remedy this with some other mathematically convenient equation of state is not an adequate response; one must try to base the description of matter on a realistic model of microscopic physics or thermodynamics, and few have considered such questions [Bradley and Sviestins, 1984, Salvati et al, 1987, Bona and Coll, 1988, Romano and Pavon, 1992.…”