Chaos in pseudo-Newtonian black holes with halos

dc.creatorGueron, E
dc.creatorLetelier, PS
dc.date2001
dc.dateMAR
dc.date2014-11-17T22:24:39Z
dc.date2015-11-26T17:42:51Z
dc.date2014-11-17T22:24:39Z
dc.date2015-11-26T17:42:51Z
dc.date.accessioned2018-03-29T00:24:50Z
dc.date.available2018-03-29T00:24:50Z
dc.identifierAstronomy & Astrophysics. Edp Sciences S A, v. 368, n. 2, n. 716, n. 720, 2001.
dc.identifier0004-6361
dc.identifierWOS:000168306200034
dc.identifier10.1051/0004-6361:20010018
dc.identifierhttp://www.repositorio.unicamp.br/jspui/handle/REPOSIP/62731
dc.identifierhttp://www.repositorio.unicamp.br/handle/REPOSIP/62731
dc.identifierhttp://repositorio.unicamp.br/jspui/handle/REPOSIP/62731
dc.identifier.urihttp://repositorioslatinoamericanos.uchile.cl/handle/2250/1287421
dc.descriptionNewtonian as well as special relativistic dynamics are used to study the stability of orbits of a test particle moving around a black hole with a dipolar halo. The black hole is modeled by either the usual monopole potential or the Paczyriki-Wiita pseudo-Newtonian potential. The full general relativistic similar case is also considered. The Poincare section method and the Lyapunov characteristic exponents show that the orbits for the pseudo-Newtonian potential models are more unstable than the corresponding general relativistic geodesics.
dc.description368
dc.description2
dc.description716
dc.description720
dc.languageen
dc.publisherEdp Sciences S A
dc.publisherLes Ulis Cedex A
dc.publisherFrança
dc.relationAstronomy & Astrophysics
dc.relationAstron. Astrophys.
dc.rightsaberto
dc.sourceWeb of Science
dc.subjectchaos
dc.subjectgalaxies : halos
dc.subjectrelativity
dc.subjectinstabilities
dc.subjectcelestial mechanics, stellar dynamics
dc.subjectStellar Dynamics
dc.titleChaos in pseudo-Newtonian black holes with halos
dc.typeArtículos de revistas


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