Editing Quasinormal mode (section)

==Mathematical physics==
In [[theoretical physics]], a '''quasinormal mode''' is a formal solution of linearized [[differential equation]]s (such as the linearized equations of [[general relativity]] constraining perturbations around a [[black hole]] solution) with a complex [[eigenvalue]] ([[frequency]]).<ref>{{Cite journal|title = Quasinormal modes of black holes: From astrophysics to string theory|journal = Reviews of Modern Physics|date = 2011-07-11|pages = 793–836|volume = 83|issue = 3|doi = 10.1103/RevModPhys.83.793|first1 = R. A.|last1 = Konoplya|first2 = Alexander|last2 = Zhidenko|arxiv = 1102.4014 |bibcode = 2011RvMP...83..793K | s2cid=118735176 }}</ref><ref>{{Cite journal|title = Quasi-Normal Modes of Stars and Black Holes|journal = Living Reviews in Relativity|date = 1999-01-01|first1 = Kostas D.|last1 = Kokkotas|first2 = Bernd G.|last2 = Schmidt| volume=2 | issue=1 | page=2 | doi=10.12942/lrr-1999-2 | doi-access=free | pmid=28191830 | pmc=5253841 | arxiv=gr-qc/9909058 | bibcode=1999LRR.....2....2K }}</ref>

[[Black hole]]s have many quasinormal modes (or 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.