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Taub–NUT space
Exact solution to Einstein's equations From Wikipedia, the free encyclopedia
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The Taub–NUT metric (/tɔːb nʌt/,[1] /- ˌɛn.juːˈtiː/) is an exact solution to Einstein's equations. It may be considered a first attempt in finding the metric of a spinning black hole. It is sometimes also used in homogeneous but anisotropic cosmological models formulated in the framework of general relativity.[citation needed]
![]() | This article may be too technical for most readers to understand. (January 2025) |
The underlying Taub space was found by Abraham Haskel Taub (1951), and extended to a larger manifold by Ezra T. Newman, Louis A. Tamburino, and Theodore W. J. Unti (1963), whose initials form the "NUT" of "Taub–NUT".
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Description
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Taub's solution is an empty space solution of Einstein's equations with topology R×S3 and metric (or equivalently line element)
where
and m and l are positive constants.
Taub's metric has coordinate singularities at , and Newman, Tamburino and Unti showed how to extend the metric across these surfaces.
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Related work
Kerr metric
When Roy Kerr developed the Kerr metric for spinning black holes in 1963, he ended up with a four-parameter solution, one of which was the mass and another the angular momentum of the central body. One of the two other parameters was the NUT-parameter, which he threw out of his solution because he found it to be nonphysical since it caused the metric to be not asymptotically flat,[2][3] while other sources interpret it either as a gravomagnetic monopole parameter of the central mass,[4] or a twisting property of the surrounding spacetime.[5]
Misner spacetime
A simplified 1+1-dimensional version of the Taub–NUT spacetime is the Misner spacetime.
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References
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