Stability of five-dimensional rotating black holes projected on the brane

Berti, E; Kokkotas, KD; Papantonopoulos, E

dc.contributor.author	Berti, E	en
dc.contributor.author	Kokkotas, KD	en
dc.contributor.author	Papantonopoulos, E	en
dc.date.accessioned	2014-03-01T01:19:33Z
dc.date.available	2014-03-01T01:19:33Z
dc.date.issued	2003	en
dc.identifier.issn	0556-2821	en
dc.identifier.uri	https://dspace.lib.ntua.gr/xmlui/handle/123456789/15573
dc.subject	Continued Fraction	en
dc.subject	Extreme Value	en
dc.subject	Quasinormal Modes	en
dc.subject	4 dimensional	en
dc.subject	Angular Momentum	en
dc.subject	Black Hole	en
dc.subject.classification	Astronomy & Astrophysics	en
dc.subject.classification	Physics, Particles & Fields	en
dc.subject.other	PARTICLE EMISSION RATES	en
dc.subject.other	QUASI-NORMAL MODES	en
dc.subject.other	MASSLESS PARTICLES	en
dc.subject.other	SPACE-TIMES	en
dc.subject.other	DIMENSIONS	en
dc.subject.other	MILLIMETER	en
dc.subject.other	UNIQUENESS	en
dc.subject.other	HIERARCHY	en
dc.subject.other	LHC	en
dc.title	Stability of five-dimensional rotating black holes projected on the brane	en
heal.type	journalArticle	en
heal.identifier.primary	10.1103/PhysRevD.68.064020	en
heal.identifier.secondary	http://dx.doi.org/10.1103/PhysRevD.68.064020	en
heal.identifier.secondary	064020	en
heal.language	English	en
heal.publicationDate	2003	en
heal.abstract	We study the stability of five-dimensional Myers-Perry black holes with a single angular momentum under linear perturbations, and we compute the quasinormal modes of the black hole metric projected on the brane, using Leaver's continued fraction method. In our numerical search we do not find unstable modes. The damping time of the modes having l = m = 2 and l = m = 1 tends to infinity as the black hole spin tends to the extremal value, showing a behavior reminiscent of the one observed for ordinary four-dimensional Kerr black holes. © 2003 The American Physical Society.	en
heal.publisher	AMERICAN PHYSICAL SOC	en
heal.journalName	Physical Review D	en
dc.identifier.doi	10.1103/PhysRevD.68.064020	en
dc.identifier.isi	ISI:000185830200051	en
dc.identifier.volume	68	en
dc.identifier.issue	6	en