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| Recently, the properties of ]s have been tested in the context of the ]. Also, the asymptotic behavior of quasinormal modes was proposed to be related to the ] in ], but convincing arguments have not been found yet. | Recently, the properties of ]s have been tested in the context of the ]. Also, the asymptotic behavior of quasinormal modes was proposed to be related to the ] in ], but convincing arguments have not been found yet. | ||
| See also ]. | ==See also== | ||
| * ]. | |||
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Revision as of 05:07, 13 February 2005
In theoretical physics, a quasinormal mode is a formal solution of linearized differential equations (such as the linearized equations of general relativity constraining perturbations around a black hole solution) with a complex eigenvalue (frequency).
Black holes have many quasinormal modes (also: ringing modes) that describe the exponential decrease of asymmetry of the black hole in time as it evolves towards the perfect spherical shape.
Recently, the properties of quasinormal modes have been tested in the context of the AdS/CFT correspondence. Also, the asymptotic behavior of quasinormal modes was proposed to be related to the Immirzi parameter in loop quantum gravity, but convincing arguments have not been found yet.
See also
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