The Kerr black hole hypothesis: a review of methods and results
Abstract
While a general, powerful framework for testing and constraining gravity theories in the weak field, slow-moving regime exists for several decades (the parametrized post-Newtonian formalism), an analogous experimental and theoretical framework to test the strong-field and strong-curvature regime of gravity is still being developed. One of the most remarkable strong-field predictions of Einstein’s General Theory of Relativity is the Kerr black hole hypothesis. It states that all astrophysical black holes in isolation are described by the Kerr solution, and therefore completely defined by just two parameters: their mass and angular momentum. In this paper we discuss a family of parametrically deformed Kerr spacetimes and study the relative importance of dierent order parameters. We construct a generalization of this spacetime and study the importance of the dierent types of parameters, and argue that neither of the metrics can be mapped to rotating black hole solutions in alternative theories of gravity even in the limit of small parameters and slow rotation.
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