Quasi-Normal Modes and Exponential Energy Decay for the Kerr-de Sitter Black Hole

We provide a rigorous definition of quasi-normal modes for a rotating black hole. They are given by the poles of a certain meromorphic family of operators and agree with the heuristic definition in the physics literature. If the black hole rotates slowly enough, we show that these poles form a discrete subset of $${\mathbb C}$$ . As an application we prove that the local energy of linear waves in that background decays exponentially once orthogonality to the zero resonance is imposed.

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