The spacetime metric is, in Boyer-Lindquist coordinates,
This represents the exact solution to General relativity/Einstein equations for the stress-energy tensor for an electromagnetic field from a charged rotating black hole. In the case that the charge is zero it becomes an exact vacuum solution to Einstein's field equations and is called just "the Kerr solution".
There are three important mathematical surfaces for this line element, the static limit and the inner and outer event horizons. The static limit is the outermost place something can be outside the outer horizon with a zero angular velocity. It is
The event horizons are coordinate singularities in the metric where .
The outer event horizon is at
and the inner horizon is at
An external observer can never see an event at which something crosses into the outer horizon. A remote observer reckoning with these coordinates will reckon that it takes an infinite time for something infalling to reach the outer horizon even though it takes a finite proper time till the event according to what fell in.
Penrose diagram for coordinate extension of a charged or rotating black hole
Above we see a Penrose diagram representing a coordinate extension (1) for a charged or rotating black hole. The same way as mapping Schwarzschild coordinates onto Kruskal-Szekeres coordinate reveals two seperate external regions for the Schwarzschild black hole, such a mapping done for a charged or rotating hole reveals an even more multiply connected region for charged and rotating black holes. Lets say region I represents our external region outside a charged black hole. In the same way that the other external region is inaccessible as the wormhole connection is not transversible, external region II is also not accessible from region I. The difference is that there are other external regions VII and VIII which are ideed accessible from region I by transversible paths at least one way. One should expect this as the radial movement case of geodesic motion for a neutral test particle written above leads back out of the hole without intersecting the physical singularity at .