Non-Linear Effects in Non-Kerr spacetimes

Understand

There is a chance that the spacetime around massive compact objects which are expected to be black holes is not described by the Kerr metric, but by a metric which can be considered as a perturbation of the Kerr metric.

• These non-Kerr spacetimes are also known as bumpy black hole spacetimes.
• We expect that, if some kind of a bumpy black hole exists, the spacetime around it should possess some features which will make the divergence from a Kerr spacetime detectable.
• One of the differences is that these non-Kerr spacetimes do not posses all the symmetries needed to make them integrable.