Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6404
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dc.contributor.authorSamuel, J.-
dc.date.accessioned2016-09-26T11:57:56Z-
dc.date.available2016-09-26T11:57:56Z-
dc.date.issued2016-01-
dc.identifier.citationClassical and Quantum Gravity, 2016, Vol.33, p015006en_US
dc.identifier.issn0264-9381-
dc.identifier.issn1361-6382 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/6404-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractWick rotation is usually performed by rotating the time coordinate to imaginary values. In a general curved spacetime, the notion of a time coordinate is ambiguous. We note here, that within the tetrad formalism of general relativity, it is possible to perform a Wick rotation directly in the tangent space using considerably less structure: a timelike, future pointing vector field, which need not be killing or hypersurface orthogonal. This method has the advantage of yielding real Euclidean metrics, even in spacetimes which are not static. When applied to a black hole exterior, the null generators of the event horizon reduce to points in the Euclidean spacetime. Requiring that the Wick rotated holonomy of the null generators be trivial ensures the absence of a 'conical singularity' in the Euclidean space. To illustrate the basic idea, we use the tangent space Wick rotation to compute the Hawking temperature by Euclidean methods in a few spacetimes including the Kerr black hole.en_US
dc.language.isoenen_US
dc.publisherIOP Publishing Ltd.en_US
dc.relation.urihttp://arxiv.org/abs/1510.07365en_US
dc.relation.urihttp://dx.doi.org/10.1088/0264-9381/33/1/015006en_US
dc.relation.urihttp://adsabs.harvard.edu/abs/2016CQGra..33a5006Sen_US
dc.rights2016 IOP Publishing Ltd.en_US
dc.subjectEuclidean methodsen_US
dc.titleWick rotation in the tangent spaceen_US
dc.typeArticleen_US
Appears in Collections:Research Papers (TP)

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