Homogeneous viscous universes with magnetic field I. Basic equations

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…”

“…With respect to the existence of limit sets, we first make a proposition about the late-time dynamics of the system: Proposition 1.-Consider the dynamical system (14) with parameters in the region S1ðFÞ defined by À1 w < 1 3 , 0 ¼ 0, and 0 ¼ 0. Then, as !…”

“…In Ref. [14] van Leeuwen and Salvati studied the dynamics of general Bianchi class A models containing a magneto-viscous fluid and a large-scale magnetic field. Banerjee and Sanyal [15] presented some exact solutions of Bianchi types I and III cosmological models consisting of a viscous fluid and an axial magnetic field.…”

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].…”

Bianchi type-III non-static magnetized cosmological model for perfect fluid distribution in general relativity

“…Cosmological models with an incident magnetic field for various Bianchi types have been investigated by several authors viz. Zel'dovich (1965), Doroshkevich (1965), Tupper (1977), Damiao Soares (1978), Tsoubelis (1979), Dunn and Tupper (1980), Lorentz (1980aLorentz ( , 1980bLorentz ( , 1982, Spokoiny (1981Spokoiny ( , 1982, Roy et al (1985), Van Leeuwen (1985), Ribeiro and Sanyal (1987), Nayak and Bhuyan (1987). Roy and Banerjee (1997) have investigated a Bianchi type II cosmological model of Petrov type D representing an imperfect fluid with a source free magnetic field.…”