A matrix method for quasinormal modes: Kerr and Kerr-Sen black holes

dc.contributorUniv Fed Itajuba
dc.contributorChina West Normal Univ
dc.contributorUniversidade de São Paulo (USP)
dc.contributorUniversidade Estadual Paulista (Unesp)
dc.date.accessioned2018-11-26T17:56:02Z
dc.date.available2018-11-26T17:56:02Z
dc.date.created2018-11-26T17:56:02Z
dc.date.issued2017-08-20
dc.identifierModern Physics Letters A. Singapore: World Scientific Publ Co Pte Ltd, v. 32, n. 25, 9 p., 2017.
dc.identifier0217-7323
dc.identifierhttp://hdl.handle.net/11449/164773
dc.identifier10.1142/S0217732317501346
dc.identifierWOS:000406720800007
dc.description.abstractIn this paper, a matrix method is employed to study the scalar quasinormal modes of Kerr as well as Kerr-Sen black holes. Discretization is applied to transfer the scalar perturbation equation into a matrix form eigenvalue problem, where the resulting radial and angular equations are derived by the method of separation of variables. The eigenvalues, quasinormal frequencies omega and angular quantum numbers lambda, are then obtained by numerically solving the resultant homogeneous matrix equation. This work shows that the present approach is an accurate, as well as efficient method for investigating quasinormal modes.
dc.languageeng
dc.publisherWorld Scientific Publ Co Pte Ltd
dc.relationModern Physics Letters A
dc.relation0,650
dc.rightsAcesso restrito
dc.sourceWeb of Science
dc.subjectKerr black hole
dc.subjectKerr-Sen black hole
dc.subjectquasinormal modes
dc.subjectTaylor series
dc.subjectTeukolsky equation
dc.titleA matrix method for quasinormal modes: Kerr and Kerr-Sen black holes
dc.typeArtículos de revistas


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