Journal
COMMUNICATIONS IN MATHEMATICAL PHYSICS
Volume 306, Issue 1, Pages 119-163Publisher
SPRINGER
DOI: 10.1007/s00220-011-1286-x
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Funding
- NSF [DMS-0654436]
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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 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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