A Radiating and Rotating Metric

A non-static solution of Einstein's field equations of General Relativity representing the gravitational field of an axisymmetric radiation flow is obtained using the Eddington or the Kerr-Schild form for the metric. A solution obtained here manifestly corresponds to the Kerr metric with its mass-parameter, $m$, being an arbitrary function of the advanced (retarded) null-time coordinate. Then, when $m$ is constant, the solution reduces to the standard Kerr metric expressed in terms of the used null coordinate. Further, when the angular momentum parameter, $a$, a constant here, is set to zero, the solution reduces to the Vaidya metric expressed in terms of the used null-coordinate.