We present here an interior solution of the Einstein-Maxwell equations for a charged static fluid sphere. The physical 3-space t = constant of the solution is spheroidal. The solution is interpreted as an exact relativistic model for a charged superdense star.

The Einstein field equations have been solved for Bianchi type VI 0 spacetimes with viscous fluid source. Four cosmological models are derived. They have nonzero expansion and shear. One of them have nonzero constant shear viscosity coefficient.

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Using the method of differential forma a Kerr-like metric is derived aa ah exact solution of Einstein's field equationB corresponding to & perfect fluid distribution plus a pure radiation field. The solution ia interpreted aa a Kerr-like radiating metric in the cosmological background of an expanding universe. The radiating Kerr metric and the radiating ~ssociated Kerr metric are derived aa particular cMes. The details of the solution are also discussed.