Non-Linear Effects in Non-Kerr spacetimes
arXiv:1408.4697 · doi:10.1007/978-3-319-06761-2_16
Abstract
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. We discuss how we can take advantage of this fact by examining EMRIs into the Manko-Novikov spacetime.
8 pages, 3 Figures; to appear in the proceedings of the conference "Relativity and Gravitation: 100 Years after Einstein in Prague" (2012)
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- Chaotic motion of scalar particle coupling to Chern-Simons invariant in Kerr black hole spacetime
- Slowly-rotating compact objects: the nonintegrability of Hartle-Thorne particle geodesics
- Chaotic Behavior of Geodesics in Kerr-like Spacetime
- Chaotic motion of particles around a dyonic Kerr-Newman black hole immersed in the Melvin-swirling universe