Birth of a quasi-stationary black hole in an outcoupled Bose–Einstein condensate

Nova, Juan Ramón Muñoz de; Guéry-Odelin, David; Sols, Fernando; Zapata, I.

doi:10.1088/1367-2630/16/12/123033

Cited by 14 publications

(36 citation statements)

References 53 publications

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“…[40], where the reader is referred for more details. A detailed discussion of gravitational analogues and the mean-field formalism for Bose-Einstein condensates is presented in Appendix A.…”

Section: Black Hole In An Outcoupled Bose-einstein Condensate Thrmentioning

confidence: 99%

“…The remaining free (without confining potential) region L + L lat x will be denoted as the supersonic or downstream region, since we expect the escaping flow there to be sufficiently dilute to be supersonic. Although in theory the supersonic region is infinite, in numerical computations it must be finite; for that purpose, and also to reduce spurious numerical artifacts, absorbing boundary conditions (ABC) are implemented in the downstream region [40].…”

Section: Black Hole In An Outcoupled Bose-einstein Condensate Thrmentioning

confidence: 99%

“…Specifically, the length of the optical lattice is chosen such that it contains a discrete number of periods, n osc , L lat ≡ n osc d. After rescaling the condensate wave function as Ψ(x, t) → √ n 0 Ψ(x, t), the actual degrees of freedom of the system are neatly revealed; once the initial chemical potential is fixed, only L/ξ 0 , d/ξ 0 , τ /t 0 , V 0 /µ 0 , V ∞ /µ 0 and n osc are free parameters of the problem. However, for typical values of the magnitudes, the features of the system depend very weakly on (L/ξ 0 , τ /t 0 , V 0 /µ 0 , n osc ) [40]. The major role played by V ∞ /µ 0 and d/ξ 0 comes from their determining the asymptotic band structure of the optical lattice in the quasi-stationary regime because, as well known, the spectrum of any periodic potential is understood in terms of gaps and energy bands.…”

Section: A Ideal Optical Latticementioning

confidence: 99%

“…For ζ ≪ 1 we are in the nearly-free atom regime, where bands are wide and gaps are narrow, while for ζ ≫ 1 we have the opposite tight-binding regime, with narrow and widely spaced bands. In practice, only the lowest energy band is needed to understand the dynamics of the system [40].…”

Section: A Ideal Optical Latticementioning

confidence: 99%

“…2: (i) initial chemical potential µ 0 slightly above the bottom of the final conduction band, E min ; (ii) sufficiently wide asymptotic conduction band. This last condition can be understood as the optical lattice acting like a low-pass filter, with the band width being the equivalent of the cutoff frequency, since the higher the cutoff, the wider is the transmission band and then more small waves on top of the condensate travel away through the optical lattice, reducing the spatial fluctuations of the local chemical potential [40]. As V ∞ µ 0 , wide bands imply that we are in the nearly-free atom limit, ζ ≪ 1, in which one can write analytical formulas for the bottom and the top of the lowest energy band, respectively:…”

Section: A Ideal Optical Latticementioning

confidence: 99%

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Quantum Transport in the Black‐Hole Configuration of an Atom Condensate Outcoupled Through an Optical Lattice

2017

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The outcoupling of a Bose-Einstein condensate through an optical lattice provides an interesting scenario to study quantum transport phenomena or the analog Hawking effect as the system can reach a quasi-stationary black-hole configuration. We devote this work to characterize the quantum transport properties of quasi-particles on top of this black-hole configuration by computing the corresponding scattering matrix. We find that most of the features can be understood in terms of the usual Schrödinger scattering. In particular, a transmission band appears in the spectrum, with the normal-normal transmission dominating over the anomalous-normal one. We show that this picture still holds in a realistic experimental situation where the actual Gaussian envelope of the optical lattice is considered. A peaked resonant structure is displayed near the upper end of the transmission band, which suggests that the proposed setup is a good candidate to provide a clear signal of spontaneous Hawking radiation.

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Section: Black Hole In An Outcoupled Bose-einstein Condensate Thrmentioning

confidence: 99%

Section: Black Hole In An Outcoupled Bose-einstein Condensate Thrmentioning

confidence: 99%

Section: A Ideal Optical Latticementioning

confidence: 99%

Section: A Ideal Optical Latticementioning

confidence: 99%

Section: A Ideal Optical Latticementioning

confidence: 99%

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Quantum Transport in the Black‐Hole Configuration of an Atom Condensate Outcoupled Through an Optical Lattice

2017

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Observation of stationary spontaneous Hawking radiation and the time evolution of an analogue black hole

et al. 2021

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We observe the time dependence of the Hawking radiation in an analogue black hole. Soon after the formation of the horizon, there is little or no Hawking radiation. The Hawking radiation then ramps up during approximately one period of oscillation, until it reaches the quantity expected for spontaneous emission. This is similar to a black hole created from gravitational collapse. The spectrum remains approximately constant at the spontaneous level for some time, similar to a stationary black hole. An inner horizon then forms, in analogy with a charged black hole. The inner horizon causes stimulated Hawking radiation. Both types of stimulation predicted by Ted Jacobson and coworkers likely contribute, but the monochromatic stimulation probably contributes more than does the black-hole lasing.

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Observation of thermal Hawking radiation and its temperature in an analogue black hole

Nova

Golubkov

Kolobov

et al. 2019

Nature

308

301

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We measure the correlation spectrum of the Hawking radiation emitted by an analogue black hole and find it to be thermal at the Hawking temperature implied by the analogue surface gravity. The Hawking radiation is in the regime of linear dispersion, in analogy with a real black hole. Furthermore, the radiation inside of the black hole is seen to be composed of negative-energy partners only. This work confirms the prediction of Hawking's theory regarding the value of the Hawking temperature, as well as the thermality of the spectrum. The thermality of Hawking radiation is the root of the information paradox. The correlations between the Hawking and partner particles imply that the analogue black hole has no analogue firewall.It was a profound realization that the entropy of a black hole [1] and Hawking radiation [2,3] should have the same temperature, within a numerical factor on the order of unity. It was further asserted that Hawking radiation should have a thermal spectrum, which creates an information paradox [4,5]. Furthermore, it was proposed that the physics of Hawking radiation could be verified in an analogue system [6]. This proposal was carefully studied and developed theoretically [7][8][9][10][11][12][13][14][15][16][17][18][19]. Classical white and black-hole analogues were also studied experimentally [20][21][22][23], as well as a variety of other analogue gravitational systems [24][25][26][27][28][29][30]. The theoretical works, combined with our long-term study of this subject [14,[31][32][33][34], allowed for the observation of spontaneous Hawking radiation in an analogue black hole [35]. Several theoretical works studied our observation [35], and made predictions about the thermality and Hawking temperature [36][37][38][39][40]. During the years since our observation [35], we have made many improvements to the experimental apparatus. This allows us to study the thermality of the Hawking spectrum, and compare its temperature with the prediction given by the analogue of the surface gravity. In this work, we find that the spectrum of Hawking radiation agrees well with a thermal spectrum, and its temperature is given by Hawking's prediction.The analogue black hole consists of a flowing Bose-Einstein condensate. The flow velocity out in the region < 0 is less than the speed of sound out , as indicated in Fig. 1a. This region corresponds to the outside of the black hole. For > 0, the flow is supersonic ( in > in ),

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Birth of a quasi-stationary black hole in an outcoupled Bose–Einstein condensate

Cited by 14 publications

References 53 publications

Quantum Transport in the Black‐Hole Configuration of an Atom Condensate Outcoupled Through an Optical Lattice

Quantum Transport in the Black‐Hole Configuration of an Atom Condensate Outcoupled Through an Optical Lattice

Observation of stationary spontaneous Hawking radiation and the time evolution of an analogue black hole

Observation of thermal Hawking radiation and its temperature in an analogue black hole

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