Unstable fields in Kerr spacetimes

We show that both the interior region r < M − √M² − a² of a Kerr black hole and the a² > M² Kerr naked singularity admit unstable solutions of the Teukolsky equation for any value of the spin weight. For every harmonic number, there is at least one axially symmetric mode that grows exponential...

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Detalles Bibliográficos
Autores principales:	Dotti, Gustavo, Gleiser, Reinaldo J., Ranea Sandoval, Ignacio Francisco
Formato:	Articulo
Lenguaje:	Inglés
Publicado:	2012
Materias:	Astronomía Gravity in more than four dimensions, Kaluza-Klein theory, unified field theories; alternative theories of gravity Classical general relativity Physics of black holes Gravitational waves
Acceso en línea:	http://sedici.unlp.edu.ar/handle/10915/132154
Aporte de:	SEDICI (UNLP) de Universidad Nacional de La Plata

id	I19-R120-10915-132154
record_format	dspace
institution	Universidad Nacional de La Plata
institution_str	I-19
repository_str	R-120
collection	SEDICI (UNLP)
language	Inglés
topic	Astronomía Gravity in more than four dimensions, Kaluza-Klein theory, unified field theories; alternative theories of gravity Classical general relativity Physics of black holes Gravitational waves
spellingShingle	Astronomía Gravity in more than four dimensions, Kaluza-Klein theory, unified field theories; alternative theories of gravity Classical general relativity Physics of black holes Gravitational waves Dotti, Gustavo Gleiser, Reinaldo J. Ranea Sandoval, Ignacio Francisco Unstable fields in Kerr spacetimes
topic_facet	Astronomía Gravity in more than four dimensions, Kaluza-Klein theory, unified field theories; alternative theories of gravity Classical general relativity Physics of black holes Gravitational waves
description	We show that both the interior region r < M − √M² − a² of a Kerr black hole and the a² > M² Kerr naked singularity admit unstable solutions of the Teukolsky equation for any value of the spin weight. For every harmonic number, there is at least one axially symmetric mode that grows exponentially in time and decays properly in the radial directions. These can be used as Debye potentials to generate solutions for the scalar, Weyl spinor, Maxwell and linearized gravity field equations on these backgrounds, satisfying appropriate spatial boundary conditions and growing exponentially in time, as shown in detail for the Maxwell case. It is suggested that the existence of the unstable modes is related to the so-called time machine region, where the axial Killing vector field is timelike, and the Teukolsky equation, restricted to axially symmetric fields, changes its character from hyperbolic to elliptic.
format	Articulo Articulo
author	Dotti, Gustavo Gleiser, Reinaldo J. Ranea Sandoval, Ignacio Francisco
author_facet	Dotti, Gustavo Gleiser, Reinaldo J. Ranea Sandoval, Ignacio Francisco
author_sort	Dotti, Gustavo
title	Unstable fields in Kerr spacetimes
title_short	Unstable fields in Kerr spacetimes
title_full	Unstable fields in Kerr spacetimes
title_fullStr	Unstable fields in Kerr spacetimes
title_full_unstemmed	Unstable fields in Kerr spacetimes
title_sort	unstable fields in kerr spacetimes
publishDate	2012
url	http://sedici.unlp.edu.ar/handle/10915/132154
work_keys_str_mv	AT dottigustavo unstablefieldsinkerrspacetimes AT gleiserreinaldoj unstablefieldsinkerrspacetimes AT raneasandovalignaciofrancisco unstablefieldsinkerrspacetimes
bdutipo_str	Repositorios
_version_	1764820455980531712

Unstable fields in Kerr spacetimes

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