In this work we are mostly interested in uniqueness results for four-dimensional black holes. This leads us
naturally to consider those vacuum Kaluza–Klein spacetimes with enough symmetries to lead to
four-dimensional spacetimes after dimensional reduction, providing henceforth four-dimensional black holes.
It is convenient to start with a very short overview of the subject; the reader is referred to [101, 172
] and
references therein for more information. Standard examples of Kaluza–Klein black holes are
provided by the Schwarzschild metric multiplied by any spatially flat homogeneous space (e.g.,
a torus). Non-trivial examples can be found in [272, 211]; see also [200, 172] and reference
therein.
http://www.livingreviews.org/lrr-2012-7 |
Living Rev. Relativity 15, (2012), 7
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