Rotating Topological Black Holes

Details Rotating Topological Black Holes Rotating Topological Black Holes

1997-10-28

arxiv.org/abs/gr-qc/9710123v2

Phys.Rev.D57:6127-6137,1998; Erratum-ibid.D60:109902,1999

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

25 pages, LateX, five ps figures added, minor errors corrected, addition of new references, improved discussion of the conserv

Scientific paper

10.1103/PhysRevD.57.6127

A class of metrics solving Einstein's equations with negative cosmological constant and representing rotating, topological black holes is presented. All such solutions are in the Petrov type-$D$ class, and can be obtained from the most general metric known in this class by acting with suitably chosen discrete groups of isometries. First, by analytical continuation of the Kerr-de Sitter metric, a solution describing uncharged, rotating black holes whose event horizon is a Riemann surface of arbitrary genus $g > 1$, is obtained. Then a solution representing a rotating, uncharged toroidal black hole is also presented. The higher genus black holes appear to be quite exotic objects, they lack global axial symmetry and have an intricate causal structure. The toroidal blackholes appear to be simpler, they have rotational symmetry and the amount of rotation they can have is bounded by some power of the mass.

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