Scattering of sound waves by a canonical acoustic hole

Dolan, Sam R.; Oliveira, Érika Arantes de; Crispino, Luís C. B.

doi:10.1103/physrevd.79.064014

Cited by 52 publications

(62 citation statements)

References 40 publications

(69 reference statements)

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“…For example, the angular width of the 'glory' diffraction pattern that arises from the scattering of a monochromatic wave [42] is related to the Regge pole spectrum [52,53] (though it was shown [42] that the glory effect is much weaker for a CAH than a similarly-sized Schwarzschild hole). Finally, we hope that the simple methods used here may also be applied to other analogue systems of experimental interest in future.…”

Section: Discussionmentioning

confidence: 99%

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Quasinormal modes and Regge poles of the canonical acoustic hole

2010

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We compute the quasinormal mode frequencies and Regge poles of the canonical acoustic hole (a black hole analogue), using three methods. First, we show how damped oscillations arise by evolving generic perturbations in the time domain using a simple finite-difference scheme. We use our results to estimate the fundamental QN frequencies of the low multipolar modes l = 1, 2, . . .. Next, we apply an asymptotic method to obtain an expansion for the frequency in inverse powers of l + 1/2 for low overtones. We test the expansion by comparing against our time-domain results, and (existing) WKB results. The expansion method is then extended to locate the Regge poles. Finally, to check the expansion of Regge poles we compute the spectrum numerically by direct integration in the frequency domain. We give a geometric interpretation of our results and comment on experimental verification.

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Section: Discussionmentioning

confidence: 99%

“…Geodesics were considered in detail in a previous study of scattering by the CAH [42]. We recall the key results below.…”

Section: Geodesicsmentioning

confidence: 99%

Quasinormal modes and Regge poles of the canonical acoustic hole

2010

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“…The numerical method used here is analogous to the one described in Ref. [28]. We have employed an iterative method similar to that used in Refs.…”

Section: Arxiv:09053339v1 [Gr-qc] 20 May 2009mentioning

confidence: 99%

Electromagnetic Wave Scattering by Schwarzschild Black Holes

2009

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We analyze the scattering of a planar monochromatic electromagnetic wave incident upon a Schwarzschild black hole. We obtain accurate numerical results from the partial wave method for the electromagnetic scattering cross section, and show that they are in excellent agreement with analytical approximations. The scattering of electromagnetic waves is compared with the scattering of scalar, spinor and gravitational waves. We present a unified picture of the scattering of all massless fields for the first time.PACS numbers: 04.40.-b, 04.70.-s, 11.80.-m Black holes are thought to be efficient catalysts for the liberation of rest-mass energy. As such, black holes are implicated in the most energetic phenomena in the known universe (e.g. gamma ray bursts). On the other hand, after a turbulent youth, many black holes settle into a quiescent old age. Some estimates suggest there may be up to a billion quiescent stellar-mass black holes within our galaxy [1]. Their existence may be inferred from, for example, the transient lensing of background sources; a handful of events have so far been observed [2]. A possibility for future consideration is that quiescent black holes may be indirectly identified from the 'fingerprint' they leave on radiation that impinges upon them.Over the last four decades, some clues about the properties of any such 'fingerprint' have been uncovered. For example, a time-dependent perturbation incident upon a black hole will excite characteristic damped ringing in response. The frequencies and decay rates of the ringing are linked to the well-studied quasinormal mode spectrum [3]. Black holes illuminated by long-lasting planar radiation will create interference patterns, and rotating black holes will create distinctive polarization patterns [4]. Both effects depend strongly on the ratio of horizon size to wavelength. Hence, it is conceivable that future gravitational-wave detectors may be able to identify the fingerprint from rapid and distinctive variations across a narrow frequency band. Nevertheless, inferring the presence of quiescent black holes from such clues must remain a challenge for future decades.Scattering by black holes is of foundational interest in both black hole physics [5] and scattering theory [6]. Many authors have studied the simplest timeindependent scenario, in which a black hole is subject to a long-lasting, monochromatic beam of radiation. Here, the key dimensionless quantity is the ratio r h /λ where r h is the horizon size of the black hole, and λ is the wavelength of the incident wave. The interference pattern depends also on the spin s of the perturbing field, with s = 0, 1/2, 1 and 2 corresponding to scalar, neutrino, electromagnetic and gravitational fields, respectively.To the best of our knowledge, the first paper outlining a calculation of wave scattering cross section in the spacetime of a black hole was published by Matzner [7] in the late sixties. Since then, planar wave scattering from black holes has received much attention, especially in Schwarzschild and...

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“…It is therefore of interest to understand if a given property observed in BH spacetimes can be mimicked by analogue models. Within this context, BH properties like absorption [4,5], scattering [6,7], quasinormal modes, and Regge poles [8][9][10][11][12] have been investigated in acoustic analogue spacetimes over the past few years.…”

Section: Introductionmentioning

confidence: 99%

Acoustic clouds: Standing sound waves around a black hole analogue

et al. 2015

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Under certain conditions sound waves in fluids experience an acoustic horizon with analogue properties to those of a black hole event horizon. In particular, a draining bathtub-like model can give rise to a rotating acoustic horizon and hence a rotating black hole (acoustic) analogue. We show that sound waves, when enclosed in a cylindrical cavity, can form stationary waves around such rotating acoustic holes. These acoustic perturbations display similar properties to the scalar clouds that have been studied around Kerr and Kerr-Newman black holes; thus they are dubbed acoustic clouds. We make the comparison between scalar clouds around Kerr black holes and acoustic clouds around the draining bathtub explicit by studying also the properties of scalar clouds around Kerr black holes enclosed in a cavity. Acoustic clouds suggest the possibility of testing, experimentally, the existence and properties of black hole clouds, using analog models.

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Scattering of sound waves by a canonical acoustic hole

Cited by 52 publications

References 40 publications

Quasinormal modes and Regge poles of the canonical acoustic hole

Quasinormal modes and Regge poles of the canonical acoustic hole

Electromagnetic Wave Scattering by Schwarzschild Black Holes

Acoustic clouds: Standing sound waves around a black hole analogue

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