Quasinormal Modes and Late-Time Tails of Canonical Acoustic Black Holes

Abstract

In this paper, we investigate the evolution of classical wave propagation in the canonical acoustic black hole by numerical method and discuss the details of tail phenomenon. The oscillating frequency and damping time scale both increase with the angular momentum $l$. For the lower $l$, numerical results show the lowest WKB approximation gives the most reliable result. We also find that time scale of the interim region from ringing to tail is not affected obviously by changing $l$.

arXiv comment5 pages, 6 figures

References in corpus (9)

• Acoustic black holes: horizons, ergospheres, and Hawking radiation
• Quasinormal behavior of the D-dimensional Schwarzshild black hole and higher order WKB approach
• Wave Propagation in Gravitational Systems: Late Time Behavior
• Quasinormal modes and classical wave propagation in analogue black holes
• Hawking radiation in an electro-magnetic wave-guide?
• Quasinormal modes of Schwarzschild black holes in four and higher dimensions
• Gravitational quasinormal modes for Kerr Anti-de Sitter black holes
• Quasinormal modes of stringy black holes
• Object Picture of Quasinormal Modes for Stringy Black Holes

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• Resonant frequencies of a massless scalar field in the canonical acoustic black hole spacetime
• Analytical expression for a class of spherically symmetric solutions in Lorentz breaking massive gravity
• Gravitational analog of the canonical acoustic black hole in Einstein-scalar-Gauss-Bonnet theory