The Kerr Metric is a solution to the equations of general relativity that describes the geometry of spacetime around a rotating black hole. It was discovered by mathematician Roy P. Kerr in 1963 and is significant because it extends the Schwarzschild solution, which describes non-rotating black holes, to include angular momentum. In the Kerr Metric, the black hole is characterized by two parameters: its mass and its angular momentum. This solution reveals unique features, such as the existence of an "ergosphere," where objects cannot remain in place due to the intense rotation of the black hole.