]>PLB34560S0370-2693(19)30240-010.1016/j.physletb.2019.04.008TheoryFig. 1(a): Dimensionless density |ϕ|2/ρ0 as a function of z/l⊥ and ω⊥t, obtained for the initial position ζ0 = 0, phase ϕ0 ≈ −0.86 rad, and the dissipation rate γ ≈ 0.22 × 10−4 (corresponding to the temperature T ≈ 5 nK) by numerically solving the SGPE. Inset: Intensity of the dark soliton at t = 0 (blue dashed line) and t ≈ 300 ms (red solid line). (b) and (c): Dark soliton's width (red squares) and blackness (black circles) as functions of ω⊥t for T ≈ 5 nK (b) and as functions of T for t ≈ 600 ms (c). Error bars indicate the standard deviation from the mean value for 50 runs. The red dashed (black dashed-dotted) lines stand for the asymptotic behavior of the dark soliton's width (blackness) predicted by Eq. (5). (d): The variance of the position of the center of the dark soliton, D(ζDS), as a function of ω⊥t obtained from the numerical simulation (red triangles) and from the analytic prediction (6) (black solid line). Left lower inset: D(ζDS) (black solid line) and its linear part (blue dashed line) in the range of 0 < ω⊥t < 5. Right upper inset: The dependence of ζDS on T for t ≈ 600 ms.Fig. 1Fig. 2(a): The setup scheme for mimicking sonic black hole, with notations defined in the text. (b) and (c): Bogoliubov spectrum of the linear excitations (phonons) on the background flow in the upstream (a) and downstream (b) of the BEC. The Mach number in the upstream (downstream) is mu = v0u/|cs,u| ≈ 0.3 < 1 (md = v0d/|cs,d| ≈ 2.3 > 1). Red dashed-dotted lines denote the slope (sound speed) of long-wavelength phonon excitation near k = 0. “in” and “out” denote in-going and out-going directions with respect to the black hole horizon, respectively.Fig. 2Fig. 3The scheme for detecting the analogue HR in the BEC. (a): A cigar-shaped BEC (with length ≈500 μm and flow velocity v0 = 0.25 mm s−1) passes over the change of radial confinement at z = 0, allowing the occurrence of the black hole horizon and the analogue HR. (b): When the uniform density region of the BEC reaches the horizon t = 0, a dark soliton is generated in the upstream. (c) and (d): The diffusion of the dark soliton due to the influence of the HR at ω⊥,ut = 300 (t ≈ 359 ms) (c) and 600 (t ≈ 718 ms) (d), respectively. Middle row: Dimensionless density |ϕ|2/ρ0u along the z direction, corresponding to (a)-(d), where the white and shaded regions denote the upstream and the downstream, respectively. Lower row: The first panel shows the velocity of the whole BEC at ω⊥,ut = −300, 0, 300, 600, and 900 (t ≈ −359, 0, 359, 718, and 1077 ms). The rest panels zoom in the dark solitons. δ1 (δ2) in the last panel denotes the distance between the soliton center and its left (right) border.Fig. 3Soliton diffusion in a Bose-Einstein condensate: A signature of the analogue Hawking radiationChaoHangac⁎chang@phy.ecnu.edu.cnGregoryGabadadzebcGuoxiangHuangacaState Key Laboratory of Precision Spectroscopy, School of Physical and Material Sciences, East China Normal University, Shanghai 200062, ChinaState Key Laboratory of Precision SpectroscopySchool of Physical and Material SciencesEast China Normal UniversityShanghai200062ChinabDepartment of Physics, New York University, New York, NY 10003, USADepartment of PhysicsNew York UniversityNew YorkNY10003USAcNYU-ECNU Institute of Physics at NYU Shanghai, Shanghai 200062, ChinaNYU-ECNU Institute of Physics at NYU ShanghaiShanghai200062China⁎Corresponding author at: State Key Laboratory of Precision Spectroscopy, School of Physical and Material Sciences, East China Normal University, Shanghai 200062, China.State Key Laboratory of Precision SpectroscopySchool of Physical and Material SciencesEast China Normal UniversityShanghai200062ChinaEditor: M. CvetičAbstractThe analog Hawking radiation (HR) emanating from a sonic black hole horizon formed in a cigar-shaped Bose-Einstein condensate (BEC) at finite temperature is investigated. In particular, we study the effect of HR on a dark (topological) soliton. We show that, due to thermal fluctuations, the dark soliton in the BEC displays a nonlinear Brownian motion resulting in a specific asymmetric diffusion. Based on numerical simulations we argue that the analog HR formed in the BEC can be detected indirectly through measurement of the dark soliton diffusion.KeywordsAnalog Hawking radiationSolitonsBose-Einstein condensation1IntroductionThe goal of this work is to propose a scheme for an indirect detection of the analog Hawking radiation in a certain quantum system, using a topological soliton that the same system supports.Hawking radiation (HR) is a quantum effect in a classical background of a black hole [1]. It has been a subject of numerous studies aimed at better understanding of the fundamental principles of quantum physics in the presence of a black hole (BH) geometry (see, e.g., [2] and references therein).In a commonly discussed astrophysical setting – i.e., for a BH in the center of a galaxy – the intensity of HR is negligible as compared to that of the in/out-flows triggered by accretion of surrounding matter and radiation onto the BH. Hence, detection of HR in such settings appears to be unlikely.It is then desirable to look for different setups in which similar quantum radiation, in otherwise classical background, might be expected and detected. Such a program had been initiated by Unruh who noticed the equivalence between the equations used to predict HR and those governing wave propagation in certain inhomogeneous and moving media [3]. The radiation of quantum counterparts of such waves, potentially accessible in a lab, is referred as the analog HR.A numerous interesting platforms have been proposed for the detection of the analogue HR [4–24]. Among them, atomic Bose-Einstein condensates (BECs) were suggested as potentially useful for the explorations. Moreover, a direct observation of the analog HR has recently been claimed in such systems [25–28].Given the complexity of such experiments and subtleties of the detection [25–28], it is highly desirable to have complementary methods of observing effects of HR in BEC's. For instance, indirect detection by observing influence of HR on object within BEC that can be controlled and manipulated would be welcome. In this work we propose one such scheme using peculiarities of diffusion of a topological (dark) soliton in BEC caused by a thermal radiation, the analog HR in our case.Solitons are fascinating large-amplitude excitations, stabilized by the interplay between nonlinearity and dispersion/diffraction. They appear in nonlinear media or in nonlinear relativistic systems. Among diverse types of solitons discovered in many branches of physics, matter wave solitons in atomic BECs have been broadly studied [29–40]. Their diffusion has also been explored recently in various settings [41–44].In this work we use the accumulated knowledge on the analog HR, on solitons, and on field theory techniques describing both of these phenomena, to investigate the HR driven diffusion of dark (topological) solitons in a cigar-shaped atomic BEC with a repulsive atom-atom interaction.By developing an analytic approach based on effective field theory methods, we show that a dark soliton immersed in BEC displays a nonlinear temporal variance of its position under the influence of thermal fluctuations, corresponding to a nonlinear Brownian motion. Thus, it exhibits an apparent, asymmetric diffusion during its propagation. In particular, we find that the width and depth of the dark soliton change in time t respectively as, t3/2T and t−3/2/T, with T being temperature of thermal radiation. Using these results, we propose a scheme for an indirect detection of HR by measuring the diffusion of the soliton caused by the analog HR emanating from a sonic black hole horizon in a moving BEC.The proposed scheme is entirely based on the inherent nonlinearity of the BEC, and by that, it differs from previous studies. Since the dark soliton can be regarded as a large classical particle, its diffusion should be easier to detect than it is to detect the Hawking quanta directly.2The modelWe consider a cigar-shaped atomic BEC with repulsive atom-atom interaction that is trapped by the potential Vext(r)=M2[ω⊥2(x2+y2)+ωz2z2], where M is the atomic mass and ω⊥ (ωz) is transverse (axial) harmonic oscillator frequency, with ω⊥≫ωz. At low energies and momenta the dynamics of such BEC can be described by an effective Lagrangian for a space-time dependent order parameter of the condensed state, ψ(z,t), that can be referred as a wave-function of the condensate. In the long-wavelength approximation both the condensate and its fluctuations are captured by a classical solution for ψ(z,t) and its perturbations. Below we will directly deal with the equation of motion that follows from the effective Lagrangian, and also incorporates the terms due to the external harmonic trap. Thus, the wave-function ψ(z,t), satisfies the Gross-Pitaevskii (GP) equation:iħ∂ψ∂t=(−ħ22M∂2∂z2+M2ωz2z2+ħω⊥+g1D|ψ|2)ψ, where g1D≡2ħω⊥as, with as>0 is the s-wave scattering length determined by the quartic repulsive self-interaction term in the effective Lagrangian [45]. The condensate solution and spectrum of its long-wavelength perturbations (the Bogliubov spectrum of phonons) are well known; we just emphasize for further use how that spectrum changes when one looks at a background flow of BEC with velocity v0 along the z directionω=v0k±[k22M(ħ2k22M+2g1Dρ0)]1/2, where “+” (“−”) corresponds to the phonon propagating in the +z (−z) direction, while ρ0 is the one-dimensional density. The sound phase velocity at low momentum reads (ω/k)k=0=v0+cs, where cs=±g1Dρ0/M is the sound speed in the BEC frame.The above description does not capture the effects of finite temperature. In particular, at any nonzero temperature a finite fraction of the atoms will not be in the condensed state and will scatter incoherently off the condensed atoms, leading to dissipation in the condensate. Furthermore, thermal fluctuations will give rise to randomness. To account for both of these effects in a parametric way one modifies the GP equation into a stochastic GP equation (SGPE) [47,48](1)iħ∂ϕ∂t=(1−iγ)(−ħ22M∂2∂z2+M2ωz2z2+ħω⊥+g1D|ϕ|2)ϕ+η(z,t), where γ≡iβħΣK(z,t)/4 is the dissipation rate (with β=1/(kBT) and kB the Boltzmann constant), and ħΣK is the Keldysh self-energy due to the incoherent collisions between condensed and noncondensed atoms [49]. The last term η parametrizes the thermal fluctuation, obeying the fluctuation-dissipation relation〈η(z,t)η⁎(z′,t′)〉=2ħkBTγ(z,t)δ(z−z′)δ(t−t′), with 〈⋯〉 denoting the averaging over different noise realizations. Since the BEC is highly elongated and the region of interest is far away from the edges, an approximate space- and time-independent dissipation rate can be used in the analytical treatment, i.e., we adopt the approximation γ≈γ(0)=3MkBTas2/(πħ2) [50].For convenience of later calculations, we rewrite the SGPE (1) into the dimensionless form(2)i∂F∂τ=(1−iγ)(1−μ˜−ik˜0∂∂ζ−12∂2∂ζ2+Ω22ζ2+g|F|2)F+Λ, where τ=ω⊥t, ζ=l⊥−1z, g=2asρ0, F=ϕeiμ˜τ−ik˜0ζ+iω˜0τ/ρ0, Ω=ωz/ω⊥≪1, μ˜=μ/(ħω⊥), and Λ=ηeiμ˜τ−ik˜0ζ+iω˜0τ/(ħω⊥), with l⊥≡ħ/(Mω⊥) being the transverse harmonic-oscillator length, k˜0=k0l⊥ being the flow wavenumber, and ω˜0=ω0/ω⊥ [ω0≡Mv02/(2ħ)] the flow frequency. The correlator of the dimensionless fluctuation fields reads 〈Λ⁎(ζ,τ)Λ(ζ′,τ′)〉=2kBTγδ(ζ−ζ′)δ(τ−τ′)/(ħω⊥2).If γ, Ω, Λ vanish, then the dimensionless SGPE (2) admits an exact dark soliton solution [51]F=(μ˜−1)/g(cosϕ0tanhZ˜+isinϕ0), with Z˜=μ˜−1cosϕ0[ζ−(k˜0+μ˜−1sinϕ0)τ−ζ0]. Here, ζ0 denotes the initial position of the soliton center and ϕ0 (|ϕ0|<π/2) is a phase characterizing the blackness (the difference between the minimum soliton intensity and the background intensity) as [(μ˜−1)/g]cos2ϕ0, its width 3.3/(μ˜−1cosϕ0), and its velocity k˜0+μ˜−1sinϕ0.In the next section we will consider small but nonzero γ, Ω, and Λ, and their effects on the soliton.3Diffusion of the solitonWe start by looking for analytical results on soliton diffusion, to get a clear physical picture and then to compare with numerical simulations. Starting with the SGPE (1) in a weak nonlinear regime a stochastic Korteweg-de Vries (KdV) equation can be derived by using the multi-scale method developed in Ref. [52]; the result reads as follows:(3)∂u∂τ+3c˜su0u∂u∂ζ˜−18c˜s∂3u∂ζ˜3=−14c˜s∂Λ∂ζ˜−R(u,γ), where ζ˜=ζ−(k˜0+c˜s)τ and u=Fexp(−iφ)−u0 [46]. The first term on the right hand side of Eq. (3) results from the thermal fluctuation; the second term, R, comes from the higher-order effects – e.g., the high-order thermal fluctuations, higher-order dispersion and nonlinearity, the trapping potential along the z direction, etc. – which are all small and neglected in the analytical treatment, but will be included in our numerical simulations.If Λ is set to zero, then Eq. (3) admits an exact dark soliton solution u=−A0sech2[2c˜s2A0/u0(ζ˜+c˜sA0τ/u0−ζ0)], where A0 is a positive constant characterizing the amplitude of the soliton. In the leading-order approximation the dark soliton solution of Eq. (3) can be expressed asF(ζ,τ)=u0[1−A˜0sech2(2c˜s2A˜0X)]eiφ, with A˜0=A0/u0, X=ζ−[k˜0+c˜s(1−A˜0)]τ−ζ0, and φ=−2A˜0tanh(2c˜s2A˜0X). We should note that: (i) only the small-amplitude dark solitons can be described by the KdV equation; (ii) dark solitons can be at rest in the lab frame if k˜0+c˜s(1−A˜0)=0, which can only be satisfied if there is a background flow (i.e. k˜0≠0).If the thermal fluctuations are weak enough (Λ≪1), the first term on the right hand side of Eq. (3) can be treated as a small perturbation. Thus, its effect on the dark soliton can be studied by perturbing the non-perturbative soliton solution [53]; this leads to the following perturbed solution(4)u=−(A0+2A0W1)sech2[(2c˜s2A˜0+c˜su0W1)X+W2], with W1=[1/(2u0)]∫0τdτ′∫−∞∞dsΛtanhssech2s, and W2=(c˜s2A˜0/u0)∫0τdτ′∫0τ′dτ″∫−∞∞dsΛtanhssech2s−[1/(2u02A˜0)]×∫0τdτ′∫−∞∞dsΛ(ssinhs−coshs)/cosh3s.In what follows we'll be interested in the long-time behavior of the dark soliton under the influence of the thermal fluctuations. To this end, we compute the ensemble average 〈u〉, and consider the case of τ≫1. Following the method of Ref. [54], and using the relations 〈W12〉=u02Λ0σ/(15c˜s4), 〈W1W2〉=2u02A0Λ0σ2/(15c˜s4), and 〈W22〉=u02Λ0σ/(15c˜s4)[(30+π2)/(24A0)+4A02σ2], we obtain the asymptotic solution for τ≫1(5)〈u〉=−u05/43πc˜s103Λ0τ3exp(−5u03A˜0Λ0τ3X2), where Λ0≡2kBTγ/(ħω⊥2)∝T2. From Eq. (5) we see that for a long-time diffusion, the width of the dark soliton grows as t3/2T while the blackness decreases as 1/(t3/2T). Even though the soliton gets deformated because of the diffusion, the area enclosed by its shape-function remains constant.The obtained soliton diffusion is due to its Brownian motion induced by the thermal fluctuation in the BEC. From the solution (4), we can easily extract the time dependence of the position of the center of the soliton, ζDS=ζ0+[k˜0+c˜s(1−A˜0)]τ−u0W2/[c˜s(2A0+W1)]. From this, we can calculate the variance of the position, D(ζDS)≡〈(ζDS−〈ζDS〉)2〉, which reads(6)D(ζDS)≈1u0(30+π245116c˜s4A˜02+215A˜0τ2)Λ0τ. We see that for small τ, D(ζDS)∝τ, in accordance with the Einstein relation for Brownian motion [55]; however for larger τ, D(ζDS)∝τ3, that is, the dark soliton displays a nonlinear time-variance of its position, which can be regarded as a nonlinear Brownian motion. Furthermore, in contrast with the Einstein relation where the diffusion coefficient ∝1/γ, here D(ζDS)∝γ since the dark soliton has a negative mass [43,44].Having the theoretical part clarified we adopt realistic parameters based on a recent experiment reported in Ref. [33], where a cigar-shaped almost pure 87Rb BEC of N≈5×104 atoms in the 〈52S1/2,F=1,mF=−1〉 state was prepared, with (ω⊥,ωz)=2π×{133,5.9} Hz and the peak density around 5.8×1013 cm−3. Furthermore, the velocity of the background flow is taken to be v0≈0.7mms−1, and the temperature of the BEC is assumed to be T≈5 nK (which is much lower than the critical temperature of one-dimensional BEC, Tc=Nħωz/[ln(2N)kB]≈1.2 μK [56]). With the above parameters at hand, one calculates l⊥≈1 μm, cs≈±0.8mms−1, and γ≈0.22×10−4.To test the obtained analytical results, we solve the SGPE numerically by using the spectral method together with the fourth-order Runge-Kutta method for time stepping. The numerical evolution of a typical dark soliton is shown in Fig. 1(a), with the initial position and phase respectively taken as ζ0=0 and ϕ0≈−0.86 rad (the initial blackness and width are approximately 0.6 and 4.3, respectively). Fig. 1(b) shows the width (red squares) and the blackness (black circles) of the dark soliton as functions of τ for T≈5 nK, obtained by averaging over 50 runs of independent noise realizations. The respective analytic curves obtained are also shown by the red dashed and black dashed-dotted lines, respectively. We see that the numerical results agree with the analytic ones for large τ, however, a disagreement occurs for small τ since the asymptotic solution (5) is valid only in the long-time regime (i.e. τ≫1). Fig. 1(c) shows the same quantities as functions of T for τ=500 (t≈600 ms). Since τ≫1, the numerical results agree well with the analytic predictions in the entire range of T.The dependence of D(ζDS) on τ is illustrated in Fig. 1(d), where the red triangles are obtained from the numerical calculation and the black solid line is the analytic result (6). One can see that the numerical and analytic results are matched quite well. The left lower inset of the figure shows D(ζDS) (black solid line) and its linear part (blue dashed line) in the range of 0≤τ≤5. One sees that they are matched only for a very short time, 0<τ≲2 (0<t≲2.4 ms). Thus, for a long-time behavior, the dark soliton displays a nonlinear Brownian motion instead of a linear one. The dependence of ζDS on T for τ=500 (t≈600 ms) is also given, as shown in the right-upper inset.4Detection on analogue HR via soliton diffusionWe now turn to demonstrate that the measurement of the dark soliton diffusion might be an effective technique to detect the analogue HR in the BEC. To this end, we assume that the background flow in the BEC is generated along the z direction; this can be realized by, say, adiabatically accelerating the trapping potential in the z direction until the BEC reaches a constant velocity v0 [25]. The near-horizon geometry of an analogue sonic black hole can be mimicked by a transition region from a subsonic to supersonic background flow [see Fig. 2(a)]. If the central position of the horizon is at z=0, the upstream (downstream) of the BEC corresponds to the region z<0 (z>0), where the flow is subsonic (supersonic). The analog HR is a thermal radiation of the phonons emanating from the analog horizon. Since the background flow is supersonic in the downstream region, and the phonons cannot escape from it, that region can be regarded as the interior of an analog black hole.In practice, to create a horizon of the analogue black hole, we assume there is a stationary, step-like change of the radial confinement of the trapping potential, i.e. ω⊥=ω⊥,u for z<0 and ω⊥=ω⊥,d for z>0, with ω⊥,u<ω⊥,d (hereafter, subscripts “u” and “d” refer to the upstream and downstream, respectively). Accordingly, the transverse harmonic-oscillator length in the upstream (downstream) is l⊥,u≡ħ/(Mω⊥,u) (l⊥,d≡ħ/(Mω⊥,d)). The quantities in the upstream and downstream regions can be related to one another by the mass-current conservation and the condition of equal chemical potential in the whole BEC [17]: ρ0uv0u=ρ0dv0d, and M2v0u2+ħω⊥,u+g1D,uρ0u=M2v0d2+ħω⊥,d+g1D,dρ0d, respectively, with g1D,u=2ħω⊥,uas and g1D,d=2ħω⊥,das.The sonic black hole requires that v0u<|cs,u| and v0d>|cs,d|, where the sound speeds in the upstream (downstream) is cs,u=±g1D,uρ0u/M (cs,d=±g1D,dρ0d/M). For a simple case with v0u=|cs,u|−u and v0d=|cs,d|+u (0<u≪|cs,u|,|cs,d|), the analogue Hawking temperature is determined by the velocity gradient (see, e.g., [25])TH≈ħ2πkB|∂∂z(v−cs)|≈ħuπkBl0, where l0=ħ/(M|cs|) is the healing length. The latter is assumed to be the shortest length scale in the hydrodynamical limit where the wavelength of the Bogoliubov excitations are much longer than l0 [57].For the numerical calculations, we take as=94.8a0, ω⊥,u=2π×133 Hz (l⊥,u≈0.94 μm), ω⊥,d=2π×140 Hz (l⊥,d≈0.91 μm), ρ0u≈1.0×106 cm−1, v0u=0.25mms−1, and cs,u≈±0.78mms−1. With the above parameters we get ρ0d≈2.67×105 cm−1, v0d≈0.94mms−1, and cs,d≈±0.41mms−1. Thus, the Mach number in the upstream (downstream) reads: mu=v0u/|cs,u|≈0.3<1 (md=v0d/|cs,d|≈2.3>1), u≈0.5mms−1, and the Hawking temperature TH≈1.4 nK.Fig. 2(b) and Fig. 2(c) show the Bogoliubov spectrum in the upstream and downstream regions, respectively. We see that long-wavelength excitations in the upstream are able to propagate in both directions, i.e., they'd be in-going and out-going with respect to the horizon. However, they are dragged away by the background flow and are unable to propagate back to the black hole horizon in the downstream, i.e. they can only propagate along the out-going direction with respect to the horizon. The minimum wavelength of the trapped, long-wavelength excitations in the downstream is approximately 5.5 μm.Since the system is essentially one-dimensional, we assume that a uniform density region will quickly equilibrate at the Hawking temperature TH, as long as the latter is higher than the ambient temperature of the BEC. Once this happens, a dark soliton will be injected in the upstream region, somewhat close to the horizon, but in a way for it not to back-react on the analog horizon significantly; this can be done by employing the known phase-imprinting laser field [33], allowing to precisely set the soliton position, blackness, and velocity.If TH is higher than the temperature of all other reservoirs that may exist, the dark soliton will behave as a nonlinear Brownian particle due to the influence of the HR, as detailed in the previous section. Note that the coolest BEC realized up to now can have temperatures as low as ∼10 pK [58]. In such setups the role of the BEC thermal fluctuations will indeed be negligible and only the HR will remain responsible for the soliton diffusion. Furthermore, since the dark soliton is set with zero initial velocity [when taking A˜0=k˜0u/c˜s,u+1≈0.24 (c˜s,u<0)] and a small amplitude, it is “slow”, and hence sensitive to the influence of the HR.Last but not least, we perform the numerical simulation of the entire process of detection of the analogue HR. In the simulation, we first let the BEC (with the length ≈500 μm and a background flow velocity v0=0.25mms−1) to undergo the change in the radial confinement at z=0, enabling the emergence of the analogue black hole horizon [Fig. 3(a)]. As soon as the uniform density region reaches the horizon, a dark soliton with zero initial velocity is injected in the upstream (we set this time as t=0) [Fig. 3(b)]. Shown in Fig. 3(c) and Fig. 3(d) are numerical results on the HR-induced-diffusion of the dark soliton at τ≈300 (t≈359 ms) and τ≈600 (t≈718 ms), respectively. From Fig. 3(c), we see that the soliton width (blackness) has increased (decreased) by nearly 1.5 times as compared with the initial values. These changes are in good agreement with the results given in Fig. 2(b), and should be possible to measure in a realistic experiment (see the third panel in the middle row of Fig. 3). In Fig. 3(d), an asymmetric soliton diffusion is observed. Specifically, we measure the distance between the soliton center and its left (right) “edge”, denoted by δ1 (δ2). We find that δ1/δ2≈1.3>1 (the last panel in the lower row of Fig. 3). Such an asymmetric soliton diffusion might be caused by the inhomogeneous density of the BEC along the longitudinal direction or by an asymmetry in the pressure acting on the soliton due to the HR. Furthermore, we calculate the velocity of the whole BEC (i.e. the velocity of the center-of-mass of the BEC), vBEC, at different times, and the influence of the HR is also calculated (see the first panel of the lower row in Fig. 3). One can see that vBEC increases from the value of the background flow velocity in the upstream to that in the downstream. Our simulation confirms that the dark soliton propagation in BEC is robust, and the soliton has the lifetime longer than 718 ms.5ConclusionThe Hawking radiation is one of the intriguing long studied quantum phenomenon in a classical background field of a black hole. Its detection in any realistic astrophysical context is unlikely. The analog Hawking radiation is governed by the mathematical equations that are identical to those used in the Hawking calculation. Therefore, it is interesting to study the analog HR in table-top experimental systems where it can be potentially detected directly or indirectly.In this work the analog HR emanating from a sonic black hole horizon formed in a cigar-shaped Bose-Einstein condensate was investigated. In particular, we studied the effect of HR on a dark (topological) soliton. We showed that under the thermal HR the dark soliton in the BEC would display a nonlinear Brownian motion resulting in a specific asymmetric diffusion. We performed numerical simulations of this process and based on the obtained results argued that the analog HR can be detected indirectly through the measurement of the dark soliton diffusion.Our scheme is complementary to the previous proposals (see works [14–17,28]) that are based on the measurements of the correlation between a pair of Hawking quanta. The method proposed and developed here may be extended to study the stochastic dynamics of other nonlinear waves [59] and other analogue gravity problems [60–68].AcknowledgementsThis work was supported by the National Natural Science Foundation of China (NSFC) under Grants Nos. 11474099 and 11475063, National Key Research and Development Program of China under Grant No. 2017YFA0304201, Shanghai Program of Shanghai Academic/Technology Research Leader under Grant No. 17XD1401500, and the US National Science Foundation under Grant No. PHY-1620039.References[1]S.W.HawkingBlack hole explosions?Nature (London)248197430S.W.HawkingParticle creation by black holesCommun. Math. Phys.431975199[2]D.MarolfThe black hole information problem: past, present, and futureRep. Prog. Phys.802017092001[3]W.G.UnruhExperimental black-hole evaporation?Phys. Rev. Lett.4619811351[4]T.A.JacobsonG.E.VolovikEvent horizons and ergoregions in 3HePhys. Rev. 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