This is an old revision of this page, as edited by Jag123 (talk | contribs) at 16:04, 19 February 2005 (ch to {{physics-stub}} - Misplaced Pages:WikiProject Stub sorting). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.
Revision as of 16:04, 19 February 2005 by Jag123 (talk | contribs) (ch to {{physics-stub}} - Misplaced Pages:WikiProject Stub sorting)(diff) ← Previous revision | Latest revision (diff) | Newer revision → (diff)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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