Acoustic black holes: horizons, ergospheres and Hawking radiation
نویسنده
چکیده
It is a deceptively simple question to ask how acoustic disturbances propagate in a non-homogeneous flowing fluid. Subject to suitable restrictions, this question can be answered by invoking the language of Lorentzian differential geometry. This paper begins with a pedagogical derivation of the following result: if the fluid is barotropic and inviscid, and the flow is irrotational (though possibly time dependent), then the equation of motion for the velocity potential describing a sound wave is identical to that for a minimally coupled massless scalar field propagating in a (3+ 1)-dimensional Lorentzian geometry 1ψ ≡ 1 √−g ∂μ (√−g g ∂νψ) = 0. The acoustic metric gμν(t,x) governing the propagation of sound depends algebraically on the density, flow velocity, and local speed of sound. Even though the underlying fluid dynamics is Newtonian, non-relativistic, and takes place in flat space plus time, the fluctuations (sound waves) are governed by an effective (3+ 1)-dimensional Lorentzian spacetime geometry. This rather simple physical system exhibits a remarkable connection between classical Newtonian physics and the differential geometry of curved (3+ 1)-dimensional Lorentzian spacetimes, and is the basis underlying a deep and fruitful analogy between the black holes of Einstein gravity and supersonic fluid flows. Many results and definitions can be carried over directly from one system to another. For example, it will be shown how to define the ergosphere, trapped regions, acoustic apparent horizon, and acoustic event horizon for a supersonic fluid flow, and the close relationship between the acoustic metric for the fluid flow surrounding a point sink and the Painlevé–Gullstrand form of the Schwarzschild metric for a black hole will be exhibited. This analysis can be used either to provide a concrete non-relativistic analogy for black-hole physics, or to provide a framework for attacking acoustics problems with the full power of Lorentzian differential geometry. PACS numbers: 0420C, 0440, 0470B, 0490, 0340G
منابع مشابه
0 Unexpectedly large surface gravities for acoustic horizons ?
Acoustic black holes are fluid dynamic analogs of general relativistic black holes, wherein the behaviour of sound waves in a moving fluid acts as an analog for scalar fields propagating in a gravitational background. Acoustic horizons, which are intimately related to regions where the speed of the fluid flow exceeds the local speed of sound, possess many of the properties more normally associa...
متن کاملUnexpectedly large surface gravities for acoustic horizons?
Acoustic black holes are fluid-dynamic analogues of general relativistic black holes, wherein the behaviour of sound waves in a moving fluid acts as an analogue for scalar fields propagating in a gravitational background. Acoustic horizons, which are intimately related to regions where the speed of the fluid flow exceeds the local speed of sound, possess many of the properties more normally ass...
متن کاملOn Hawking radiation from black rings
We calculate the quantum radiation from the five dimensional charged rotating black rings by demanding the radiation to eliminate the possible anomalies on the horizons. It is shown that the temperature, energy flux and angular-momentum flux exactly coincide with those of the Hawking radiation. The black rings considered in this paper contain the Myers-Perry black hole as a limit and the quantu...
متن کاملTransonic Black Hole Accretion as Analogue System
Classical black hole analogues (alternatively, the analogue systems) are fluid dynamical analogue of general relativistic black holes. Such analogue effects may be observed when acoustic perturbations (sound waves) propagate through a classical dissipation-less tran-sonic fluid. The acoustic horizon, which resembles the actual black hole event horizon in many ways, may be generated at the trans...
متن کاملHawking radiation from the dilatonic black holes via anomalies
Recently, Hawking radiation from a Schwarzschild-type black hole via gravitational anomaly at the horizon has been derived by Robinson and Wilczek. Their result shows that, in order to demand general coordinate covariance at the quantum level to hold in the effective theory, the flux of the energy momentum tensor required to cancel gravitational anomaly at the horizon of the black hole, is exac...
متن کامل