1 | This is no longer true if the field equations involve not only the Ricci tensor but also the Weyl tensor, such as in Lovelock theories. | |
2 | It follows that the introduction of a length scale, for instance in the form of a (negative) cosmological constant, is
a necessary condition for the existence of a black hole in ![]() |
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3 | It has been shown that this requires an infinite affine parameter distance along the null-geodesics generators of the horizon [142]. However, it may still take finite time as measured by an external observer [190]. | |
4 | This choice corresponds to rotation in the positive sense (i.e., increasing ![]() ![]() ![]() |
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5 | An alternative form was found in [140]. The relation between the two is given in [84![]() |
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6 | An equivalent system, but with a cosmological interpretation under a Wick rotation of the coordinates
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7 | The classical effective field theory of [49, 168] is an alternative to matched asymptotic expansions, which presumably should be useful as well in the context discussed in this section. | |
8 | The ![]() ![]() ![]() |
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9 | Supersymmetric solutions admit a globally defined Killing vector field that is timelike or null. The assumption is that it is non-null everywhere outside the horizon. | |
10 | The same assumption as for the ![]() ![]() |
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11 | The “topological black holes” with ![]() ![]() |
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12 | Note that topological censorship can be used to exclude the existence of topologically nonspherical black holes in
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13 | Note that this does not disagree with the stability result of [164] for ![]() ![]() |
http://www.livingreviews.org/lrr-2008-6 | ![]() This work is licensed under a Creative Commons Attribution-Noncommercial-No Derivative Works 2.0 Germany License. Problems/comments to |