The theory of Hawking radiation in laboratory analogues

Robertson, Scott

doi:10.1088/0953-4075/45/16/163001

Cited by 96 publications

(157 citation statements)

References 118 publications

(522 reference statements)

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“…Notice that a rough characterization of the curves can be obtained by considering the asymptotic behaviors of Eqs. (25) and (26), and by minimizing their sum. The symmetry with respect to interchanging A and B is then explained.…”

Section: The Other Lesson Frommentioning

confidence: 99%

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Quantum entanglement in analogue Hawking radiation: When is the final state nonseparable?

Busch

Renaud

2014

Phys. Rev. D

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We study the quantum entanglement of the quasiparticle pairs emitted by analogue black holes. We use a phenomenological description of the spectra in dispersive media to study the domains in parameter space where the final state is non-separable. In stationary flows, three modes are involved in each sector of fixed frequency, and not two as in homogeneous situations. The third spectator mode acts as an environment for the pairs, and the strength of the coupling significantly reduces the quantum coherence. The non-separability of the pairs emitted by white holes are also considered, and compared with that of black holes.

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Section: The Other Lesson Frommentioning

confidence: 99%

“…(25). The main consequence of these equations is that the non-separability can be effectively studied by considering the low frequency limit.…”

Section: Appendix B: Subluminal Dispersion Relationmentioning

confidence: 99%

Quantum entanglement in analogue Hawking radiation: When is the final state nonseparable?

Busch

Renaud

2014

Phys. Rev. D

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“…Hawking radiation is universal in the sense that the radiation does not depend on the medium. On the contrary, analogue effects depend on the physical properties of matter and such dependence gets reflected through the corresponding dispersion relation, see, e.g., Leonhardt and Robertson [2012], Robertson [2012] for further details. In existing works, however, the background space-time has been considered to be flat Minkowskian, and the configuration of the fluid (whether classical or quantum) has been assumed to follow certain simplified symmetry, like planar, circular, or spherical, for instance Barceló et al [2005].…”

Section: Discussionmentioning

confidence: 99%

Influence of the geometric configuration of accretion flow on the black hole spin dependence of relativistic acoustic geometry

Tarafdar

Das

2018

Int. J. Mod. Phys. D

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Linear perturbation of general relativistic accretion of low angular momentum hydrodynamic fluid onto a Kerr black hole leads to the formation of curved acoustic geometry embedded within the background flow. Characteristic features of such sonic geometry depend on the black hole spin. Such dependence can be probed by studying the correlation of the acoustic surface gravity κ with the Kerr parameter a. The κ − a relationship further gets influenced by the geometric configuration of the accretion flow structure. In this work, such influence has been studied for multitransonic shocked accretion where linear perturbation of general relativistic flow profile leads to the formation of two analogue black hole type horizons formed at the sonic points and one analogue white hole type horizon which is formed at the shock location producing divergent acoustic surface gravity. Dependence of the κ − a relationship on the geometric configuration has also been studied for monotransonic accretion, over the entire span of the Kerr parameter including retrograde flow. For accreting astrophysical black holes, the present work thus investigates how the salient features of the embedded relativistic sonic geometry may be determined not only by the background space-time, but also by the flow configuration of the embedding matter.

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“…[12-14, 39, 40]. The fluctuations in such equivalent photon fluids are predicted to be of the Bogolubov type [15,[41][42][43][44], and recent measurements of their dispersion relation [45] support this prediction.…”

Section: Introductionmentioning

confidence: 99%

Analog gravity by an optical vortex: Resonance enhancement of Hawking radiation

et al. 2018

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Propagation of coherent light in a Kerr nonlinear medium can be mapped onto a flow of an equivalent fluid. Here we use this mapping to model the conditions in the vicinity of a rotating black hole as a Laguerre-Gauss vortex beam. We describe weak fluctuations of the phase and amplitude of the electric field by wave equations in curved space, with a metric that is similar to the Kerr metric. We find the positions of event horizons and ergoregion boundaries, and the conditions for the onset of superradiance, which are simultaneously the conditions for a resonance in the analogue Hawking radiation. The resonance strongly enhances the otherwise exponentially weak Hawking radiation at certain frequencies, and makes its experimental observation feasible.

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The theory of Hawking radiation in laboratory analogues

Cited by 96 publications

References 118 publications

Quantum entanglement in analogue Hawking radiation: When is the final state nonseparable?

Quantum entanglement in analogue Hawking radiation: When is the final state nonseparable?

Influence of the geometric configuration of accretion flow on the black hole spin dependence of relativistic acoustic geometry

Analog gravity by an optical vortex: Resonance enhancement of Hawking radiation

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