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Accelerating black holes: Quasinormal modes and late-time tails

Kyriakos Destounis*

Rodrigo D. B. Fontana

Filipe C. Mena

  • Theoretical Astrophysics, IAAT, University of Tübingen, Auf der Morgenstelle 14, 72076 Tübingen, Germany

  • Universidade Federal da Fronteira Sul, Campus Chapecó-SC Rodovia SC 484 - Km 02, CEP 89815-899, Brazil

  • Centro de Análise Matemática, Geometria e Sistemas Dinâmicos, Instituto Superior Técnico, Universidade de Lisboa, Avenida Rovisco Pais 1, 1049-001 Lisboa, Portugal and Centro de Matemática, Universidade do Minho, 4710-057 Braga, Portugal

  • *kyriakos.destounis@uni-tuebingen.de
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Phys. Rev. D 102, 044005 – Published 4 August, 2020

DOI: https://doi.org/10.1103/PhysRevD.102.044005

Abstract

Black holes found in binaries move at very high velocities relative to our own reference frame and can accelerate due to the emission of gravitational radiation. Here, we investigate the numerical stability and late-time behavior of linear scalar perturbations in accelerating black holes described by the C-metric. We identify a family of quasinormal modes associated with the photon surface and a brand new family of purely imaginary modes associated with the boost parameter of the accelerating black hole spacetime. When the accelerating black hole is charged, we find a third family of modes which dominates the ringdown waveform near extremality. Our frequency- and time-domain analysis indicates that such spacetimes are stable under scalar fluctuations, while the late-time behavior follows an exponential decay law, dominated by quasinormal modes. This result is in contrast with the common belief that such perturbations, for black holes without a cosmological constant, always have a power-law cutoff. In this sense, our results suggest that the asymptotic structure of black hole backgrounds does not always dictate how radiative fields behave at late times.

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Phys. Rev. D 102, 044005– Published 4 August, 2020
  • Received 9 May 2020
  • Accepted 20 July 2020
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