Uniqueness of Kerr-Newman-de Sitter black holes with small angular momenta
arXiv:1702.05239 · doi:10.1007/s00023-017-0633-7
Abstract
We show that a stationary solution of the Einstein-Maxwell equations which is close to a non-degenerate Reissner-Nordström-de Sitter solution is in fact equal to a slowly rotating Kerr-Newman-de Sitter solution. The proof uses the non-linear stability of the Kerr-Newman-de Sitter family of black holes for small angular momenta, recently established by the author, together with an extension argument for Killing vector fields. Our black hole uniqueness result only requires the solution to have high but finite regularity; in particular, we do not make any analyticity assumptions.
arXiv comment10 pages, 1 figure. v2 is the published version, with updated bibliography
References in corpus (11)
- Stationary Black Holes: Uniqueness and Beyond
- A master equation for gravitational perturbations of maximally symmetric black holes in higher dimensions
- Master equations for perturbations of generalised static black holes with charge in higher dimensions
- On the uniqueness of smooth, stationary black holes in vacuum
- Uniqueness of smooth stationary black holes in vacuum: small perturbations of the Kerr spaces
- Resonance expansions for tensor-valued waves on asymptotically Kerr-de Sitter spaces
- Global analysis of quasilinear wave equations on asymptotically Kerr-de Sitter spaces
- A space-time characterization of the Kerr-Newman metric
- Rigidity of stationary black holes with small angular momentum on the horizon
- Perturbative Uniqueness of Black Holes near the Static Limit in All Dimensions
- Non-existence of multiple-black-hole solutions close to Kerr-Newman