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Simulation of Acoustic Black Hole in a Laval Nozzle

Simulation of Acoustic Black Hole in a Laval Nozzle
Simulation of Acoustic Black Hole in a Laval Nozzle

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Simulation of Acoustic Black Hole in a Laval Nozzle Hironobu Furuhashi ?and Yasusada Nambu ?Department of Physics,Graduate School of Science,Nagoya University,Nagoya 464-8602,Japan Hiromi Saida ?Department of Physics,Daido Institute of Technology,Nagoya 457-8530,Japan (Dated:March 24,2006)Abstract A numerical simulation of ?uid ?ows in a Laval nozzle is performed to observe the formation of an acoustic black hole and the classical counterpart to Hawking radiation under a realistic setting of the laboratory experiment.We aim to construct a practical procedure of the data analysis to extract the classical counterpart to Hawking radiation from experimental data.Following our procedure,we determine the surface gravity of the acoustic black hole from obtained numerical data.Some noteworthy points in analyzing the experimental data are clari?ed through our numerical simulation.PACS numbers:04.70.-s Keywords:Hawking radiation,Sonic analogue,Acoustic black hole,Laval nozzle,Classical counterpart

I.INTRODUCTION

The existence of the black hole horizon is essential to the Hawking radiation[1,2,3,4]. The horizon causes an extremely large redshift on an outgoing wave of a matter?eld during propagating from a vicinity of the horizon to the asymptotically?at region.This redshift results in the Planckian distribution of quantum mechanically created particles at the future null in?nity.Although the Hawking radiation has not yet been con?rmed observationally, it has been pointed out that the similar phenomenon appears on phonons in a transonic ?ow of a?uid.This theoretical phenomenon in the?uid is called the sonic analogue of Hawking radiation,and the transonic?uid?ow on which the sonic analogue of Hawking radiation occurs is called the acoustic black hole[5,6,7,8,9,10,11,12].In the transonic ?ow,the boundary between a subsonic and a supersonic region is the sonic point.The sonic point corresponds to the black hole horizon and called the sonic horizon.The region apart form the sonic point in the subsonic region corresponds to the asymptotically?at region in a black hole spacetime.The sound wave which propagates from a vicinity of the sonic point to the subsonic region receives the extremely large redshift and the sonic analogue of Hawking radiation appears on phonons.The Hawking temperature T H of the acoustic black hole is given by the gradient of the?uid velocity at the sonic point x=x s[5]:

T H= c

s dx v

counterpart to Hawking radiation.A candidate for the classical counterpart has already been introduced in the references[13,14]by using a Fourier component of an outgoing wave from a vicinity of the horizon.

By the way,since a realistic?uid is composed of molecules,the e?ect of the molecule size discrepancy of the?uid becomes one of the important issues of the acoustic black hole.This e?ect appears in the modi?ed dispersion relation at high energies of phonons.However,in the expansion by the molecule size discrepancy,the zeroth order form of the quantum ex-pectation value of the number operator 0|N|0 of phonons results in the thermal spectrum at least not so high energy region.That is,the e?ect of the molecule size discrepancy is not dominant in the sonic analogue of Hawking radiation.Therefore,before proceeding to the issue of the molecule size discrepancy,it is necessary to detect the ordinary Hawking radiation(thermal spectrum)by a real experiment in laboratory,and the molecule size dis-crepancy is not in the scope of this paper.Hence we concentrate on the construction of the practical procedure to extract the evidence of the Hawking radiation(thermal spectrum) from the experimental data.To do so,we make use of the classical counterpart to Hawking radiation.

We should emphasize here that the Hawking temperature(1)includes the Planck constant and we can not consider the temperature T

H

in discussing the“classical”counterpart to Hawking radiation.However we can consider the surface gravityκof the black hole horizon which is a purely classical quantity and relates to the Hawking temperature as k B T H= κ/2π.Hence,for the acoustic black hole,we consider the surface gravityκH of the sonic horizon instead of the Hawking temperature,

κH=c s d

c s

x=x s.(2)

In this paper,we aim to construct a practical procedure of the data analysis to obtain the classical counterpart to Hawking radiation in a realistic setting of the acoustic black hole.To do so,we perform a numerical simulation of a?uid?ow in a practical experimental setting,and demonstrate that our procedure works well to detect the classical counterpart to Hawking radiation.

We organize the paper as follows.In the section II,we review the acoustic black hole in a Laval nozzle and de?ne the classical counterpart to Hawking radiation.The section III is devoted to the introduction of our numerical method to simulate a transonic?ow,and

to the construction of the practical procedure of the data analysis.In the section IV,our numerical results are presented and we determine the surface gravity of the sonic horizon. Finally the summary and conclusion are in the section V.

II.ACOUSTIC BLACK HOLE WITH A LA V AL NOZZLE

We consider an acoustic black hole with a?uid in a Laval nozzle as proposed in[14].The Laval nozzle,as shown in the right panel in FIG.1,has a throat where the cross section of the nozzle becomes minimum.The?uid is accelerated from the up stream to the down stream and the?ow has the sonic point at the throat when a su?ciently large velocity is given at the inlet of the nozzle.Even if we prepare an initial?ow which has no sonic point (e.g.the lower part of the right panel in FIG.1),the?ow can settle down to a stationary transonic?ow(e.g.the upper part of the right panel in FIG.1)with appropriate boundary conditions at the inlet and the outlet of the nozzle.This is the sonic analogue model which corresponds to the gravitational collapse.

Here we note that,if a stationary transonic?ow is prepared from the beginning(which corresponds to the eternal black hole),we can not expect to obtain the classical counterpart to the Hawking radiation;for the eternal case,the tunneling of phonons across the sonic point can result in the Hawking radiation and this is the purely quantum e?ect.Hence, when we are interested in the“classical”counterpart to Hawking radiation,it is necessary to consider the situation of the sonic point formation in course of the dynamical evolution of the?uid?ow.As seen below,the sound wave which is prepared on the?uid?ow before the formation of the sonic point becomes the classical counterpart to the quantum?uctuation which causes the classical counterpart to Hawking radiation.

dρ∝ργ?1.(4) For a stationary background?ow,we can obtain the sound velocity c s and the cross section S of the nozzle as a function of the Mach number M=v/c s of the?ow:

c s=c in M2+2M2in+2M M2+2M2in+22(γ?1),(5)

where quantities with subscript “in”represent the values at the inlet of the nozzle.The spatial derivative of the Mach number at the sonic point x =x s is

dM (γ+1)

S d 2S

dx x =0=± 5

π,c s |x =0=(3|M ?|)1/6,(7)and the surface gravity given by Eq.

(2)is κH 2π 5π≈0.355.(8)

Here it should be emphasized that,because the cross section of the nozzle is set S (x )=2?cos(πx )with ?1

(8)with the surface gravity of the sonic horizon which is obtained through the observation of the classical counterpart to Hawking radiation in our numerical simulation.

FIG.2:Absolute value of the Mach number as a function of a spatial coordinate x.Each line represents the stationary solution of the?ow with di?erent boundary value M in.The blue lines represent transonic?ows.

B.Classical counterpart to Hawking radiation

As originally shown in the reference[5],the perturbation of the velocity potential for the transonic?uid?ow obeys the same equation as a massless free scalar?eld in a black hole spacetime.Therefore the classical counterpart to Hawking radiation of the acoustic black hole in the Laval nozzle should be observed by the sound wave on the transonic?uid ?ow.The most important sound wave is the one which starts to propagate against the stream from the outlet of the nozzle before the formation of the sonic point(the lower part of the right panel in FIG.1)and passes through the throat just before the moment of the sonic point formation to reach the inlet of the nozzle(the upper part of the right panel in FIG.1).This sound wave receives the extremely large redshift which will cause the classical counterpart to Hawking radiation.

When the?uid?ow is irrotational and we introduce the velocity potentialΦwhich relates with the?uid velocity as v=?xΦ,the evolution equation of the perturbationφofΦis obtained from Eqs.(3),

1

c2s [?t+v?x]φ?1

This corresponds to the Klein-Gordon equation φ=0with the acoustic metric ds2= Sρ

c s+v

,w=t+ dx

c′s0+v′0exp[?(c′s0+v′0)u],W=

1

c s (c2s?v2)exp ?2(c′s0+v′0)

c s dx

F

?UWφ=0.(14) The form of this metric near the sonic horizon is ds2≈?2S0ρ0(c′s0+v′0)dU dW,where c2s?v2≈2c s0(c′s0+v′0)x is used.This denotes explicitly that the coordinate(U,W)does not have coordinate singularities and corresponds to the Kruskal-Szekeres coordinate of the Schwarzschild spacetime.Here it should be recalled that,in the spacetime of the gravita-tional collapse(the left panel in FIG.1),the Kruskal-Szekeres coordinate is appropriate to describe the rest observer at the spacetime region before the formation of the black hole[2]. Hence the outgoing normal mode of the sound wave which corresponds to the zero point ?uctuation of the quantized matter?eld before the formation of the black hole(i.e.the mode function on the?at spacetime)is given by

φin(U)=Aφe?iω0U,(15)

whereω0is the initial frequency and Aφis the amplitude of this mode.In the original coordinate(t,x),this mode behaves as

φin(U(u))=φin(t,x)=Aφexp iω0c s+v .(16) This yields the temporal wave form at the observation point x=x obs in the asymptotic region:

φout(t)≡φin(t,x obs)=Aφexp iω0c s+v .(17) Fourier component of this mode is de?ned by

φoutω= ∞?∞dtφout(t)e iωt,(18) and the power spectrum is

P(ω)= φoutω 2= A2φeω/ωH?1(?∞<ω<+∞),(19) where the quantityωH is de?ned by

ωH≡κH2πd c

s 0.(20) Here it should be noted that,because the existence of the sonic point is assumed in the above discussion,the form of P(ω)of Eq.(19)must be obtained after the formation of the sonic horizon in the?uid?ow.

One may think it is strange that the initial frequencyω0does not appear in the power spectrum(19).It is the fact that the initial frequencyω0does appear in the power spectrum in the context of the quantum?eld theory,because the amplitude Aφis determined by the normalization condition for the mode functions to be Aφ∝1/√

the thermal distribution of the power spectrum for the sound wave of a su?ciently large amplitude in practical experiments.

As long as concerning one dimensional?uid?ow,the amplitude of the sound wave does not decrease during propagating from the outlet to the inlet of the nozzle.The one dimensional transonic?uid?ow corresponds to the two dimensional black hole spacetime in which no curvature scattering occurs.The theoretically expected power(19)is equivalent to the formula of the Hawking radiation for black holes derived ignoring the curvature scattering.

Our purpose is to observe this thermal spectrum via the numerical simulation of a tran-sonic?ow in the Laval nozzle,and to construct the practical procedure of the data analysis. Because the observable sound wave is a real valued one,we prepare the following real valued input mode at the outlet of the nozzle before the formation of the sonic horizon:

1

φin(θ)(t)=Aφcos(ω0t+θ)=

2 e?iθφin(U(t,x))+e iθφin?(U(t,x)) .(22) The e?ect of the redshift due to the formation of the acoustic black hole gradually appears on the observed sound wave.The temporal evolution of the observed sound wave is a?ected by the formation of the acoustic black hole.That is,the information of the classical counterpart to Hawking radiation is encoded in the observed sound wave.Therefore,using the output form(17),the resulting output signal after the formation of the sonic horizon is given by

1

φout(θ)(t)=

2 e?iθφoutω+e iθφout?ω .(24)

,we can not obtain the pure Fourier Hence,because the initial phaseθappears inφout(θ)

ω

componentφoutωby observing once the real valued output signalφout(θ)(t).In order to

retrieve the pure Fourier componentφoutωfrom the mixed Fourier componentφout(θ)

,we have

ω

to superpose two output modesφout(θ)andφout(θ+π/2),and obtain

φoutω=e iθ φout(θ)ω+iφout(θ+π/2)ω .(25) It is obvious that the power spectrum of this Fourier component gives the same form as Eq.(19).Therefore,in order to obtain the Planckian distribution in the power spectrum P(ω)of the observed sound wave from real valued input signals,we have to combine at least two output modes of which the input phases di?er byπ/2.

III.NUMERICAL SIMULATION OF TRANSONIC FLOWS IN A LA V AL NOZ-ZLE

Our numerical simulation is designed to generate a one dimensional transonic?uid?ow from the initial con?guration with no sonic point.We prepare the input signal at the outlet of the nozzle and observe the sound wave at the inlet of the nozzle.At the same time,the practical procedure of the data analysis is constructed.

A.Basic equations for numerical simulations

For the numerical calculation,we rewrite the?uid Eqs.(3)using c s and v,

2

v?x c s+c s?x v+ ?x S

γ?1

c s?x c s=0.(26b)

γ?1

This set of equations is not suitable for a numerical simulation of wave propagation in a transonic?ow.We transform these equations to the advection form.We introduce the Riemann invariants J±(t,x)as follows

J±≡v±2c s

8 ?x S

8 ?x S

where

V+=c s+v=γ+1

4

J?,V?=c s?v=γ?34J?.(29)

The left hand side of Eqs.(28)are of the advection form.That is,if?x S=0and?t V±=0, J+propagates upward along t? dx/V+=const.and J?propagates downward along t+ dx/V?=const.This form of the equations is suitable to treat the propagation of waves numerically.

In the sonic analogue of Hawking radiation,the perturbation of the velocity potential (sound wave)corresponds to the scalar?eld in a black hole spacetime as shown by Eq.(9). Therefore,in a practical experiment of an acoustic black hole,we should calculate the velocity potential by integrating the observed velocity of the?uid:

Φ(t,x obs)≡ x obs x0dx v(t,x),(30) where x obs is the observation point of sound waves and x0de?nes the origin of the velocity potential.However,since our experimental setting is designed to observe the sound wave at a?xed spatial point x=x obs,the observational data is a temporal sequence of v(t,x obs)and we must devise the other method to obtain the velocity potential at the observation point. In the upstream subsonic region of the transonic?ow where the e?ects of the sonic horizon is negligible and the?ow is stationary,the sound wave propagates along the“null”direction as indicated by Eq.(11)

t?

x

We make the?uid?ow against x-axis and assume v<0.The inlet of the nozzle is at x=1, the throat at x=0and the outlet at x=?1.The input wave is prepared at the outlet of the nozzle and the wave propagates against the?ow from x=?1to x=1.After the

=0at the inlet,the set of ?ow settles down to a stationary transonic?ow,since?x S|

x=1

=0at the inlet.This means that the inlet of the nozzle corresponds Eqs.(28)gives?x v|

x=1

to the asymptotically?at region in the gravitational collapse spacetime.Hence we make the observation of the sound wave at the inlet and set x obs=1.

We prepare a?ow with a homogeneous velocity distribution as the initial con?guration,

v(0,x)=V i=const.<0,c s(0,x)=1.(34) This initial con?guration of?ow has no sonic point and corresponds to the?at spacetime region before the formation of a black hole.Since our evolution equations(28)are of the advection form,it is enough to set the boundary conditions for J+at the outlet and J?at the inlet:

J+(t,?1)=J+(0,?1)+A J cos(ω0t+θ),J?(t,1)=J?(0,1)(35) where A J is a constant that represents the amplitude of the perturbation of J+at x=?1, and the values J+(0,?1)and J?(0,1)are determined consistent with Eq.(27)and Eq.(34). These boundary conditions mean that sound waves of constant amplitude continue to emerge from the outlet toward the inlet of the nozzle all the time of the numerical simulation.Here recall that the perturbationφof the velocity potentialΦplays the role of the scalar?eld in the ordinary Hawking radiation.The second term in J+(t,?1)at the outlet A J cos(ω0t+θ) causes perturbations of the velocity potential and results in the classical counterpart of Hawking radiation at the inlet of the nozzle.Because the amplitude of the sound wave in one dimensional?uid?ow does not decrease,the amplitude of the input mode of the velocity potential(21)is given by

Aφ= c s1+v1

with di?erent initial phases θ1=?π/2,θ2=0and θ3=π/2.If the amplitude A J of the perturbation part of J +is small enough,then the backreaction e?ects in the velocity potentials Φout(θi )(i =1,2,3)at the observation point (x =1)are negligible and we can subtract the common background contribution by taking the di?erence among them.Hence we obtain the Fourier components of the perturbation (sound wave)at the observation point as follows

φout(12)ω≡Φout(θ1)ω?Φout(θ2)ω=φout(θ1)ω?φout(θ2)ω

,(37a)φout(23)ω≡Φout(θ2)ω?Φout(θ3)ω=φout(θ2)ω?φout(θ3)ω,(37b)

where Φout(θi )ωis the Fourier component of Φout(θi ).These Fourier components correspond to the real valued output signal of Eq.(24).Here we

note that,according to the boundary condition (35),the perturbation parts of J +which produce the output signals of Eqs.(37)are given by

δJ (12)+=√4 ,

δJ (23)+=√4 ,(38)

where we used cos(ω0t )?cos(ω0t ±π/2)=

√2 φout(23)ω

+iφout(12)ω 2,(39)

where the factor 1/2is introduced to eliminate the factor √2A J of the input signals (38).When we carry out a realistic experiment of the acoustic black hole,the power spectrum (39)gives the classical counterpart to Hawking radiation and it has to be compared with the theoretical form (19).Hence,it is recognized that we have to perform at least three independent experiments with three di?erent input phases and observe three independent output signals to obtain the classical counterpart to Hawking radiation.

With our setting of the ?uid ?ow in the Laval nozzle,we carry out the numerical simu-lation by the ?nite di?erence method.We use the Cubic-Interpolated Pseudoparticle (CIP)method [15]for the interpolation between neighboring spatial mesh points.This method enables us to treat the shock which appears after the formation of the sonic point.We note here that the shock arises in the supersonic region and it does not a?ect the subsonic region

where we observe the output signal.The procedure of the numerical simulation to observe the thermal power spectrum (19)of

the perturbation of the velocity potential is as follows:Step 1:Generate the transonic ?uid ?ow three times with three di?erent initial phase

values,θ1=?π/2,θ2=0and θ3=π/2.Then,using Eq.(32),obtain the full velocity potentials Φout(θi )(i =1,2,3).

Step 2:Calculate the quantities φout(12)≡Φout(θ1)?Φout(θ2)and φout(23)≡Φout(θ2)?Φout(θ3).

Then compute the Fourier components of them,φout(12)ωand φout(23)ω.

Step 3:Calculate the power spectrum

P obs (ω)=1

2?ω0A J 21e ω/ωH ?1,ωH ≡κH

2π v

c s +v

,(42)and the e?ective frequency of the wave at x =1is given by ?ω0=ω0 1??c s +v .(43)The second term in Eq.(43)gives a negative contribution in our non-stationary setting of numerical experiment and the observed frequency ?ω0at x =1becomes smaller than ω0.The theoretically expected form of the power spectrum in our setting should be given by replacing ω0to ?ω0in the formula (19).

IV.NUMERICAL RESULTS

We use the parametersγ=7/5,A J=1.0×10?6andω0=100.The number of spatial mesh points are10001and the size of one mesh becomes?x=2/10001.The size of one temporal step is set?t=?x/10,and we calculate900000steps in time.The numerical simulation runs in the temporal range t=0~18.The spatial scale is normalized by L/2, where L is the length of the nozzle.The temporal scale is normalized by L/2c s(t=0),where we set c s(t=0)=1as denoted by the initial condition(34).

A.no black hole case

For the initial?uid velocity V i=?0.19,we do not observe the formation of an acoustic black hole.Figure3shows the evolution of the Mach number.After t~10,the Mach number at x=0reaches a constant value and a stationary?ow is realized.

1For FIG.6,7,13and14,we used the smaller value of the perturbation frequenctyω0=20to visualize

where v(i)denotes the?uid velocity with the input phaseθi.We can see that the sound wave propagates from x=?1to x=1.Around the throat x=0,the?uid velocity has larger value compared to the other region and the phase velocity of the outgoing wave becomes smaller.Thus the slope of the constant phase line becomes larger around the throat.

FIG.6:Spacetime distribution of˙v for V i=?0.19with A J=0,ω0=20.Colors are assigned according to the value of log|˙v|.

FIG.7:Spacetime distribution of the velocity perturbationδv≡v(2)?v(1)for V i=?0.19with A J=0,ω0=20.Colors are assigned according to the value of log|δv|.

Figure8shows the perturbation of the velocity potential at x=1.We set t0=3 in Eq.(32)to obtain the velocity potential.The observed perturbation of the velocity potential oscillates with a constant amplitude.

FIG.8:The temporal evolution of the velocity potentialφout(12)andφout(23).

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