002683806 001__ 2683806
002683806 005__ 20240211042013.0
002683806 0247_ $$2DOI$$9arXiv$$a10.1103/PhysRevD.99.104077$$qpublication
002683806 0248_ $$aoai:cds.cern.ch:2683806$$pcerncds:FULLTEXT$$pcerncds:CERN$$pcerncds:CERN:FULLTEXT
002683806 037__ $$9arXiv$$aarXiv:1901.01265$$cgr-qc
002683806 035__ $$9arXiv$$aoai:arXiv.org:1901.01265
002683806 035__ $$9Inspire$$aoai:inspirehep.net:1712386$$d2024-02-10T03:34:14Z$$h2024-02-11T03:00:06Z$$mmarcxml$$ttrue$$uhttps://inspirehep.net/api/oai2d
002683806 035__ $$9Inspire$$a1712386
002683806 041__ $$aeng
002683806 100__ $$aCardoso, Vitor$$uIST, Lisbon (main)$$uCERN$$vCENTRA, Departamento de Física, Instituto Superior Técnico—IST, Universidade de Lisboa—UL , Avenida Rovisco Pais 1, 1049 Lisboa, Portugal$$vTheoretical Physics Department, CERN 1 Esplanade des Particules, Geneva 23, CH-1211, Switzerland
002683806 245__ $$9APS$$aParametrized black hole quasinormal ringdown: Decoupled equations for nonrotating black holes
002683806 260__ $$c2019-05-29
002683806 269__ $$c2019-01-04
002683806 300__ $$a11 p
002683806 500__ $$9arXiv$$atypo corrected in Eq.(34) to match the published version
002683806 520__ $$9arXiv$$aBlack hole solutions in general relativity are simple. The frequency spectrum of linear perturbations around these solutions (i.e., the quasinormal modes) is also simple, and therefore it is a prime target for fundamental tests of black hole spacetimes and of the underlying theory of gravity. The following technical calculations must be performed to understand the imprints of any modified gravity theory on the spectrum: 1. Identify a healthy theory; 2. Find black hole solutions within the theory; 3. Compute the equations governing linearized perturbations around the black hole spacetime; 4. Solve these equations to compute the characteristic quasinormal modes. In this work (the first of a series) we assume that the background spacetime has spherical symmetry, that the relevant physics is always close to general relativity, and that there is no coupling between the perturbation equations. Under these assumptions, we provide the general numerical solution to step 4. We provide publicly available data files such that the quasinormal modes of {\em any} spherically symmetric spacetime can be computed (in principle) to arbitrary precision once the linearized perturbation equations are known. We show that the isospectrality between the even- and odd-parity quasinormal mode spectra is fragile, and we identify the necessary conditions to preserve it. Finally, we point out that new modes can appear in the spectrum even in setups that are perturbatively close to general relativity.
002683806 520__ $$9APS$$aBlack hole solutions in general relativity are simple. The frequency spectrum of linear perturbations around these solutions (i.e., the quasinormal modes) is also simple, and therefore it is a prime target for fundamental tests of black hole spacetimes and of the underlying theory of gravity. The following technical calculations must be performed to understand the imprints of any modified gravity theory on the spectrum: 1. Identify a healthy theory; 2. Find black hole solutions within the theory; 3. Compute the equations governing linearized perturbations around the black hole spacetime; 4. Solve these equations to compute the characteristic quasinormal modes. In this work (the first of a series) we assume that the background spacetime has spherical symmetry, that the relevant physics is always close to general relativity, and that there is no coupling between the perturbation equations. Under these assumptions, we provide the general numerical solution to step 4. We provide publicly available data files such that the quasinormal modes of any spherically symmetric spacetime can be computed (in principle) to arbitrary precision once the linearized perturbation equations are known. We show that the isospectrality between the even- and odd-parity quasinormal mode spectra is fragile, and we identify the necessary conditions to preserve it. Finally, we point out that new modes can appear in the spectrum even in setups that are perturbatively close to general relativity.
002683806 540__ $$3preprint$$aarXiv nonexclusive-distrib 1.0$$uhttp://arxiv.org/licenses/nonexclusive-distrib/1.0/
002683806 540__ $$3publication$$aCC-BY-4.0$$bAPS$$uhttps://creativecommons.org/licenses/by/4.0/
002683806 542__ $$3publication$$dauthors$$g2019
002683806 65017 $$2arXiv$$agr-qc
002683806 65017 $$2SzGeCERN$$aGeneral Relativity and Cosmology
002683806 690C_ $$aCERN
002683806 690C_ $$aARTICLE
002683806 700__ $$aKimura, Masashi$$uIST, Lisbon (main)$$uRikkyo U.$$vCENTRA, Departamento de Física, Instituto Superior Técnico—IST, Universidade de Lisboa—UL , Avenida Rovisco Pais 1, 1049 Lisboa, Portugal$$vDepartment of Physics, Rikkyo University , Tokyo 171-8501, Japan
002683806 700__ $$aMaselli, Andrea$$uU. Rome La Sapienza (main)$$uINFN, Rome$$vDipartimento di Fisica, “Sapienza” Università di Roma & Sezione INFN Roma1 , P.A. Moro 5, 00185 Roma, Italy
002683806 700__ $$aBerti, Emanuele$$uJohns Hopkins U. (main)$$vDepartment of Physics and Astronomy, Johns Hopkins University , 3400 North Charles Street, Baltimore, Maryland 21218, USA
002683806 700__ $$aMacedo, Caio F.B.$$uPara U.$$vCampus Salinópolis, Universidade Federal do Pará , Salinópolis, Pará, 68721-000, Brazil
002683806 700__ $$aMcManus, Ryan$$uJohns Hopkins U. (main)$$vDepartment of Physics and Astronomy, Johns Hopkins University , 3400 North Charles Street, Baltimore, Maryland 21218, USA
002683806 773__ $$c104077$$mpublication$$n10$$pPhys. Rev. D$$v99$$xPhys. Rev. D 99, 104077 (2019)$$y2019
002683806 8564_ $$81502562$$s622912$$uhttp://cds.cern.ch/record/2683806/files/10.1103_PhysRevD.99.104077.pdf$$yFulltext from Publisher
002683806 8564_ $$82225631$$s1240575$$uhttp://cds.cern.ch/record/2683806/files/1901.01265.pdf$$yFulltext
002683806 8564_ $$82225632$$s17437$$uhttp://cds.cern.ch/record/2683806/files/Fig2a.png$$y00002 Values of the frequency components $e^-_j$ (red dots) for the odd tensor modes with $\ell=2$, compared against the numerical fit of Eq.~\eqref{fitei} (black dashed curve).
002683806 8564_ $$82225633$$s16652$$uhttp://cds.cern.ch/record/2683806/files/Fig2b.png$$y00003 Values of the frequency components $e^-_j$ (red dots) for the odd tensor modes with $\ell=2$, compared against the numerical fit of Eq.~\eqref{fitei} (black dashed curve).
002683806 8564_ $$82225634$$s6406$$uhttp://cds.cern.ch/record/2683806/files/Fig1a.png$$y00000 Real and imaginary parts of the components $e^-_j$ defined in \eqref{expansionw} for $j=1,\ldots20$ and odd-parity gravitational perturbations.
002683806 8564_ $$82225635$$s6127$$uhttp://cds.cern.ch/record/2683806/files/Fig1b.png$$y00001 Real and imaginary parts of the components $e^-_j$ defined in \eqref{expansionw} for $j=1,\ldots20$ and odd-parity gravitational perturbations.
002683806 8564_ $$82225636$$s874547$$uhttp://cds.cern.ch/record/2683806/files/Fig3.png$$y00004 Contour plot for the relative errors on the parameters $\delta\omega_1$ which modifies the frequency of the $\ell=2$ fundamental BH mode. Vertical dashed lines represent configurations that lead to 20\% and 1\% fixed uncertainty. The red star identifies the values on $(\delta\omega_1,\delta\omega_2)$ for the EFT model described in Sec.~\ref{sec:EFT}.
002683806 960__ $$a13
002683806 980__ $$aARTICLE