Topological Censorship and Higher Genus Black Holes

Details Topological Censorship and Higher Genus Black Holes Topological Censorship and Higher Genus Black Holes

1999-02-20

arxiv.org/abs/gr-qc/9902061v2

Phys.Rev.D60:104039,1999

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

20 pages, Plain TeX

Scientific paper

10.1103/PhysRevD.60.104039

Motivated by recent interest in black holes whose asymptotic geometry approaches that of anti-de Sitter spacetime, we give a proof of topological censorship applicable to spacetimes with such asymptotic behavior. Employing a useful rephrasing of topological censorship as a property of homotopies of arbitrary loops, we then explore the consequences of topological censorship for horizon topology of black holes. We find that the genera of horizons are controlled by the genus of the space at infinity. Our results make it clear that there is no conflict between topological censorship and the non-spherical horizon topologies of locally anti-de Sitter black holes. More specifically, let D be the domain of outer communications of a boundary at infinity ``scri.'' We show that the principle of topological censorship (PTC), that every causal curve in D having endpoints on scri can be deformed to scri, holds under reasonable conditions for timelike scri, as it is known to do for a simply connected null scri. We then show that the PTC implies that the fundamental group of scri maps, via inclusion, onto the fundamental group of D, i.e., every loop in D is homotopic to a loop in scri. We use this to determine the integral homology of preferred spacelike hypersurfaces (Cauchy surfaces or analogues thereof) in the domain of outer communications of any 4-dimensional spacetime obeying PTC. From this, we establish that the sum of the genera of the cross-sections in which such a hypersurface meets black hole horizons is bounded above by the genus of the cut of infinity defined by the hypersurface. Our results generalize familiar theorems valid for asymptotically flat spacetimes requiring simple connectivity of the domain of outer communications and spherical topology for stationary and slowly evolving black holes.

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