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Abstract: A maximally rotating Kerr black hole is said to be extremal. In this paper weintroduce the corresponding restrictions for isolated and dynamical horizons.These reduce to the standard notions for Kerr but in general do not require thehorizon to be either stationary or rotationally symmetric. We consider physicalimplications and applications of these results. In particular we introduce aparameter e which characterizes how close a horizon is to extremality andshould be calculable in numerical simulations.



Author: Ivan Booth, Stephen Fairhurst

Source: https://arxiv.org/







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