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

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

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ap%26ss.311..401b&link_type=abstract

Astrophysics and Space Science, Volume 311, Issue 4, pp.401-406

Astronomy and Astrophysics

Astrophysics

2

Bianchi Iii, Non-Static Magnetized, Perfect Fluid

Scientific paper

We have investigated Bianchi type III non-static magnetized cosmological model for perfect fluid distribution in general relativity. We assume that F 12 is the only non-vanishing component of F ij . Maxwell’s equation partial/partial {xj}bigl(F_{{ij}}sqrt{-g}bigr)=0 leads to {F}_{12}=Ke^{-α {x}} where K and α are constants. To get a deterministic model, we assume that σ {1/1} ∝ θ which leads to A= C n where n is a constant, σ 11 the x-component of shear tensor σ ij and theta is the expansion in the model. The behaviour of the model in absence of magnetic field is discussed. The other physical and geometrical aspects of the model are also discussed.

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