A Kerr black hole is a type of rotating black hole that was first described by mathematician Roy P. Kerr in 1963. Unlike non-rotating black holes, which are spherical, Kerr black holes have an oblate shape due to their rotation. This rotation affects the space around them, creating a region called the ergosphere, where objects can gain energy and potentially escape the black hole's pull. Kerr black holes are characterized by two key properties: mass and angular momentum. They are solutions to the Einstein field equations of general relativity, which describe how mass and energy influence the curvature of space-time. These black holes are important for understanding the dynamics of rotating systems in the universe.