Acoustics
, Volume 2 (3) – Sep 8, 2020

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acoustics Article Derivation of Lighthill’s Eighth Power Law of an Aeroacoustic Quadrupole in Acoustic Spacetime Drasko Masovic * and Ennes Sarradj Technische Universität Berlin, Einsteinufer 25, 10587 Berlin, Germany; ennes.sarradj@tu-berlin.de * Correspondence: drasko.masovic@tu-berlin.de Received: 13 July 2020; Accepted: 2 September 2020; Published: 8 September 2020 Abstract: Acoustic spacetime is a four-dimensional manifold analogue to the relativistic spacetime with the reference speed of light replaced by the speed of sound. It has been established primarily for the indirect studies of relativistic phenomena by means of their better understood acoustic analogues. More recently, it has also been used for the analytical treatment of sound propagation in various uniform and non-uniform ﬂows of the background ﬂuid. In this paper the analogy is extended and utilized to derive Lighthill’s eight power law for sound generation of an aeroacoustic quadrupole. Adding to the existing analogue theory, propagating sound waves are described in terms of a weak perturbation of the background acoustic spacetime metric. The obtained result proves that the acoustic analogy can be extended to cover both weak perturbation of the ﬂuid due to the sound waves and certain sound generation mechanisms, at least in incompressible low Mach number ﬂows. Keywords: acoustic spacetime; Lighthill’s aeroacoustic analogy; quadrupole radiation 1. Introduction The fundamental work of M. J. Lighthill on aerodynamic sound and the introduction of the ﬁrst aeroacoustic analogy present a milestone in the development of aeroacoustics and acoustics in general. In his paper [1] Lighthill not only established the basis for most of the later research in aeroacoustics, but also pointed to several phenomena which were not well understood before his work: physical mechanism of sound generation by pure instability in a ﬂuid (in contrast to moving solid bodies or boundaries, which involve forces external to the ﬂuid), quadrupole sound radiation in free space, inefﬁciency of kinetic-to-acoustic energy conversion in the ﬂow of ﬂuid, and power scaling for an aeroacoustic quadrupole source, which Lighthill was able to derive even without an accurate description of the ﬂow, and its relation with the other two main types of sources—monopole and dipole. Before Lighthill’s explanation of aeroacoustic sound generation, quadrupole radiation had only a marginal importance in classical mechanics. However, parallel to the development of aeroacoustics, quadrupole radiation took a central place in the relativistic theory of gravitational waves [2], small curvatures of spacetime which cannot be generated by monopole or dipole sources. The difference between classical acoustics, deﬁned in separate Newtonian space and time, and the theory of relativity, which is based on the concept of a four-dimensional spacetime, is largely diminished by the introduction of analogue acoustic spacetime. The ﬁrst observations on the similarity between special relativity and sound propagation date back to W. Gordon [3]. Since then, Lorentz transformations have been successfully used for the problems of sound propagation in uniform mean ﬂows [4,5]. The analogy with general relativity and curved spacetime is commonly attributed to W. G. Unruh, who used it primarily for studying Hawking radiation by means of much better Acoustics 2020, 2, 666–673; doi:10.3390/acoustics2030035 www.mdpi.com/journal/acoustics Acoustics 2020, 2 667 understood acoustics in transonic ﬂows [6]. The analogy was further developed and promoted by M. Visser and C. Barceló in their studies of what is known as analogue gravity [7] or analogue models of general relativity [8]. The authors have shown that sound propagation in inhomogeneous ﬂows of the background ﬂuid can be described with differential geometry of a curved spacetime when the speed of light is replaced by the speed of sound. Different metric tensors of so deﬁned acoustic spacetime can efﬁciently capture sound propagation effects such as convection and refraction. In particular, wave operator of the Pierce equation [9] can be obtained [10] and even more general forms of metrics are discussed by Bergliaffa et al. [11]. Despite the analogy between the two analogue background spacetimes and the occurrence of quadrupole radiation in both of them in the absence of external forces, no attempts have been made to express aeroacoustic sound generation in the relativistic framework. In this work, we show that Lighthill’s power law for aeroacoustic quadrupole in an inviscid ﬂow can be derived from the acoustic spacetime analogy. Thus we also prove that the analogy can be used not merely for sound propagation, but also for aeroacoustic sound generation. In fact, since Lighthill’s analogy assumes quiescent ﬂuid outside the source region, we can consider the simplest ﬂat (Minkowski) background acoustic spacetime, which is weakly perturbed by the waves. The purely geometric perturbation representing propagating sound waves is caused by the ﬂuid motion inside the source region. The linearized relativistic theory, suitable for its description, is presented in the next section. The sound generation mechanism is considered in Section 3 and the eighth power law for the quadrupole source is obtained. Unlike Lighthill’s aeroacoustic analogy, which is an exact reformulation of the governing equations of ﬂuid dynamics, the eighth power law holds only for incompressible (low Mach number) ﬂows in the source region and in the absence of a signiﬁcant acoustic feedback. Indeed, these conditions allow a purely kinematic analogy with general relativity to be established and applied for capturing sound generation in the following analysis. Several relevant outcomes which follow from the derivation of the eighth power law from the analogy are discussed in the concluding Section 4, which also gives suggestions for future studies. 2. Waves and Motion in Acoustic Spacetime Adopting the mixed signature [ + ++], the simplest ﬂat Minkowski (acoustic) spacetime is characterized by the second-order metric tensor 2 3 1 0 0 0 6 7 0 1 0 0 6 7 ab h = 6 7 . (1) 4 0 0 1 05 0 0 0 1 Here, and in the rest of the text, Greek letters denote four-dimensional components (a, b, = 0 . . . 3, where 0 corresponds to the time coordinate) and Latin letters are used for the spatial components only (for example, i = 1 . . . 3). Therefore, x = c t, where c is the constant reference speed of 0 0 1 3 waves (here the speed of sound in the quiescent ﬂuid at inﬁnity) and x to x are spatial coordinates. The associated d’Alembertian is the classical wave operator. For a scalar f, 1 ¶ ab ,a 2 2f = h f = f = +r f, (2) ,ab ,a 2 2 ¶t 2 2 2 ¶ 1 ¶ 2 ¶ ¶ ¶ since = = and r = + + . Comma denotes usual derivative with 0 0 1 2 2 2 3 2 ¶x ¶t ¶(x ) ¶(x ) ¶(x ) respect to the coordinate which follows it (for example, f = ¶f/¶x is gradient of f) and we use ,a Einstein’s convention which implies summation over each letter appearing in an expression once as a subscript and once as a superscript [2]. The two positions of the letters correspond to the ab covariant and contravariant vector bases. Multiplication with h raises the index, as in Equation (2), Acoustics 2020, 2 668 a b while multiplication with h lowers it. Consequently, four components of vectors A and A = h A ab a ab ab are equal, apart from the time components which have opposite signs, since h = h has the ab component h = 1. Next, we suppose that the only disturbance of otherwise ﬂat spacetime outside a spatially conﬁned source region is due to propagating waves. In other words, we assume a quiescent ﬂuid with constant density r and speed of sound c through which the sound waves propagate. The total metric tensor 0 0 ab ab ab g is by deﬁnition symmetric and can be written as the sum of h and a weak component h : ab ab ab g = h + h , (3) ab with jh j 1. In the linear approximation it can be shown [2] that there always exists ab ab ab n h = h h h , (4) ab such that jh j 1 and ab h = 0. (5) ,b n ab Here, h is the trace of h and Equation (5) is called the Lorenz gauge condition. If the condition ab is not satisﬁed directly by h from Equation (4) in a certain frame, one can introduce a small change of a a a ab ab a,b b,a coordinates (gauging) x ! x + x which transforms the metric as h ! h x x such that ab ab ab n a,b b,a ab n h = h h h x x + h x (6) n ,n a a does satisfy it. For future use, we should also note that h = h and Equation (4) can be inverted to a a ab ab ab n ¯ ¯ h = h h h . (7) Relativistic equations which relate the weak perturbation of spacetime with its source, ab the stress–energy tensor T , are the linearized Einstein ﬁeld equations [2,12], 2kG ab ab 2h = T , (8) 3 2 in which dimensionless k (not to be confused with wave number) and G (in m /(kg s )) are constants. ab The instability of T , which is associated with motion of matter (or energy) in the absence of ab boundaries of spacetime, is the source of the ﬂuctuations h , which are considered to be too weak to affect the source mechanism. Such decoupling of the source and the waves it causes is in agreement with the applicability of Lighthill’s analogy, with no signiﬁcant back-reaction of sound on the ﬂow [1]. Excluding the source term at ﬁrst, the simplest solution of Equation (8) has the form of a plane wave, the real part of ab ab jk x ¯ n h = A e . (9) ab a Components of the polarization tensor A are complex constants and the four-vector k is a b a null vector in the ﬂat Minkowski spacetime: k k = h k k = 0. For example, if we suppose that a ab 3 a b the plane wave propagates in the direction of the x -axis, k = [w/c , 0, 0, w/c ], k = h k = 0 0 ab [w/c , 0, 0, w/c ], where w denotes angular frequency of the wave, and we obtain the usual exponent 0 0 n x 0 jk x = jw(t ) after replacing x with c t. Plane transverse gravitational waves are typically analyzed in the transverse-traceless gauge which suppresses the longitudinal component and leaves only two non-zero transverse components of the polarization tensor. More suitable for longitudinal acoustic waves in ﬂuids is the Newtonian gauge. The reason is that, unlike a relativistic observer, an acoustic receiver does not exist in the analogue Acoustics 2020, 2 669 acoustic spacetime, but in the Newtonian space and time. As a consequence, the Newtonian frame is preferred and only in this particular gauge the metric perturbation obtains classical acoustic meaning. In the theory of gravity such a gauge is used for calculations of the corrections of classical Newtonian gravitational potential due to relativistic phenomena. In order to show how it describes sound waves, we observe motion of a free particle in the acoustic spacetime. As in general relativity, it is given by the geodesic equation. When the particle is moving with velocity small compared to c in an essentially ﬂat spacetime, the three-dimensional acceleration equals to the lowest order [2] 2 k d x c 0 kl = h (h + h h ). (10) l0,0 0l,0 00,l dt 2 The condition for a slowly moving (non-relativistic) particle is satisﬁed by weak acoustic waves, since the particle velocity is much smaller than the speed of sound. In the Newtonian form jh j = l0 jh j jh j and therefore 0l 00 2 k 2 d x 0 ,k = h . (11) dt 2 Motion of the particle due to the wave thus depends on a single scalar h , as we expect from the longitudinal sound waves in ﬂuids. In this way we can obtain a measurable acoustic quantity (acceleration) from the acoustic spacetime analogy. It follows that the Lorenz gauge is necessary as a ab ab ¯ ¯ prerequisite for the wave equation of h , Equation (8), but once h has been obtained it has to be ab converted to h and expressed in the Newtonian gauge in order to calculate the acoustic quantities such as particle velocity and sound pressure. Nevertheless, a purely geometric quantity, the metric perturbation, sufﬁces for the description of sound waves and no dynamic analogy with linear general relativity is necessary. 3. Aeroacoustic Sound Generation In the previous section we showed how a metric perturbation captures a sound wave in the acoustic spacetime. In this section we inspect the source of waves represented by the term on the right-hand side of Equation (8). We consider only non-relativistic ﬂows in which all particles satisfy the condition j~vj c even in the source region, with ~v denoting three-dimensional particle velocity. 1 2 3 Then, the approximation U [1,~v/c ] = [1, v /c , v /c , v /c ] holds for four-velocity and the 0 0 0 0 stress–energy tensor of a perfect ﬂuid in nearly ﬂat spacetime equals [2] 2 3 2 1 2 3 r c r c v r c v r c v 0 0 0 0 0 0 0 6 7 1 1 1 1 2 1 3 6 7 r c v r v v + p r v v r v v 0 0 0 0 0 ab 6 7 T = , (12) 6 7 2 1 2 2 2 2 3 r c v r v v r v v + p r v v 4 0 0 0 0 0 5 3 1 3 2 3 3 3 r c v r v v r v v r v v + p 0 0 0 0 0 where r is matter density (here density of the background ﬂuid) and p is pressure. This stress–energy tensor satisﬁes the local conservation of mass and momentum: ab T = 0, (13) ,b which is a compact form of the laws of conservation of mass and momentum in an incompressible jk inviscid ﬂuid. We notice the similarity of the spatial part T and isentropic Lighthill’s tensor [1], which is the free-space aeroacoustic source of sound. The condition j~vj c with c the speed of 0 0 sound (which is the maximum speed in the theory) is satisﬁed in incompressible low Mach number ﬂows, which are assumed by Lighthill’s eighth power law. However, a conceptually important difference compared with Lighthill’s derivation is that we ab treat T as the source of a purely geometric perturbation of the background acoustic spacetime, not as the source of acoustic pressure or density perturbation. We do not split the conservation equations, Equation (13), into the source and propagation parts, nor do we need to select a dynamic variable Acoustics 2020, 2 670 for describing acoustic waves. Lighthill’s tensor follows from the conservation laws after the weak acoustic terms are shifted to the left-hand side of the wave equation to represent propagating sound waves. Therefore, its components are not fully conserved. In contrast to this, the entire stress–energy tensor which we consider here as the source satisﬁes the conservation laws in Equation (13). It is the source of perturbation of the spacetime itself, so it does not have to be split into the source and propagation parts in terms of dynamic quantities. In the further analysis of wave generation we follow Misner et al. [12] and consider a single isolated source, far from which the acoustic spacetime is asymptotically ﬂat towards the inﬁnity. A small metric perturbation is deﬁned in Equation (3) everywhere (including the source region) and Equation (8) holds under the condition in Equation (5). We also expect that only a small fraction of the stress–energy tensor is responsible for the radiation of waves, in accordance with the inefﬁciency of the mechanism of quadrupole radiation. Hence, it can be formally split into the dominant effective eff eff stress–energy tensor, T , and the small component t : T = T + t , and we can write ab ab ab ab ab 2kG eff 2h = (T + t ). (14) ab ab ab The general solution for both ingoing (e = 1) and outgoing (e = +1) wave is Z eff [T + t ] kG ab (teR/c ) ab 0 h = d ~y, (15) ab 2pc i i i where the integration is performed over the entire three-dimensional space and R = jx y j with x eff location of the receiver. The values of T and t are to be evaluated at the time t eR/c . ab 0 ab Next we assume that the source is compact, so that its characteristic length scale satisﬁes L c /w, where w is angular frequency of the oscillations. This actually comes down to the same slow-motion condition as above, j~vj c , since j~vj Lw. We also consider geometric far ﬁeld (R L), so we can approximate kG eff 3 h = [T + t ] d ~y, (16) ab ab (ter/c ) ab 0 2prc where r is radial coordinate of the spherical coordinate system with the compact source in its origin. From the conservation laws in Equation (13) we deduce [12] Z Z 1 d eff 3 eff 3 (T + t )x x d ~y = 2 (T + t )d ~y. (17) 00 j 00 k jk jk 2 2 c dt This important identity relates spatial components of the stress–energy tensor, which closely correspond to Lighthill’s tensor, with the component T and accordingly removes the need for a split in Lighthill’s derivation. It is possible exactly due to the fact that the full stress–energy tensor satisﬁes the conservation laws. The second-order time derivative on the left-hand side of Equation (17) takes over the role of the second-order derivatives of the source terms in Lighthill’s analogy, which naturally appear when a second-order tensor reduces to a scalar, and ultimately determines the scaling law for the quadrupole source, one of the key results of Lighthill’s original paper [1]. The integral on the left-hand side of Equation (17) represents the second moment of the mass distribution and multiplied by 1/c it is called quadrupole moment tensor of the mass distribution. It is commonly denoted with I , which is, thus, by deﬁnition jk eff 3 I = (T + t )x x d ~y. (18) jk 00 j k The quantity which appears to be more convenient for mathematical description of wave generation is reduced quadrupole moment deﬁned as Acoustics 2020, 2 671 I = I d I , (19) jk jk jk l where d is Kronecker delta. From Equations (16)–(18), jk kG d h = I (t er/c ). (20) jk jk 0 4 2 dt 4prc The assumption of geometric far ﬁeld (with respect to the characteristic length scale of the ﬂow in the source region) is necessary for simplifying the calculation with Equation (16). On the other hand, the assumption of acoustic far ﬁeld, deﬁned with respect to the sound wavelength, is not strictly necessary for estimating power of the quadrupole source. It is sufﬁcient to calculate reaction of the source to the far-ﬁeld radiation, which can be done in the acoustic near ﬁeld. Expanding h in powers jk of r for wr/c 1 (while r L) and leaving only the terms with e, which correspond to the wave radiation, gives (after replacing e = 1 for an outgoing wave) 3 5 kG d kG d react 2 h = I (t) r I (t), (21) jk jk jk 5 3 7 5 dt dt 4pc 24pc 0 0 where all higher-order terms of the series have been omitted. Using Equation (5), we can also ﬁnd 4 6 kG d kG d react k 2 k h = x I (t) r x I (t) (22) jk jk 0j 6 4 8 6 12pc dt 120pc dt 0 0 and 3 5 kG d kG d react 2 jk j k h = I (t) (r d + 2x x ) I (t) (23) 00 jj jk 5 3 7 5 12pc dt 120pc dt 0 0 These components are radiation reaction potentials given in the Lorenz gauge. The omitted terms which do not correspond to the radiation (not involving e) represent incompressible ﬂuctuations which do not propagate into the far ﬁeld. In order to calculate the Newtonian form which is suitable for obtaining classical acoustic ¯ ¯ quantities, we ﬁrst switch back to h = h h h /2 from Equation (7) and change the coordinates ab ab ab m m m as x ! x + x , with 2 4 4 kG d kG d kG d j k 2 x = I (t) + x x I (t) r I (t) (24) 0 ll jk ll 2 6 6 4 4 4 dt dt dt 12pc 48pc 48pc 0 0 0 and 3 3 kG d kG d k j x = x I (t) + x I (t). (25) j jk ll 5 3 5 3 8pc dt 24pc dt 0 0 In this gauge [12], kG d react j k h = x x I (t) (26) jk 7 5 20pc dt react react at the leading order, while the components h (wL/c )h are of higher order and negligible for 0j 00 the supposed compact source. Therefore, we obtain the metric component h in the Newtonian gauge, which describes the longitudinal perturbation of the acoustic spacetime due to the isentropic quadrupole source. Equation (26) is also one of the key results in the linearized theory of gravitation, which corrects the Newtonian gravitational potential with the contribution of gravitational wave radiation [12]. The geodesic Equation (11) gives the acceleration of a particle affected by the incoming wave: 2 l 5 d x c kG d react,l 0 j k = h = x x I (t) . (27) jk 2 5 5 dt 2 dt 40pc 0 Acoustics 2020, 2 672 We can now obtain a scaling law for the source power. Without considering details of the ﬂow in the source region, we follow Lighthill and suppose that T scales as r j~vj , where r is density of the jk 0 0 essentially incompressible ﬂow. From Equations (17)–(19),jI j r L , so the acoustic particle velocity jk from Equation (27) scales as kGr L j~v j (wL) . (28) ac Sound intensity scales as 2 2 3 4 8 k G r L j~vj 2 0 jIj r c j~v j , (29) 0 0 ac c c 0 0 where we also replac wL j~vj. Thus, we obtain the eighth power law for the acoustic power of the quadrupole source, in agreement with the result of Lighthill [1]. A more detailed comparison leads to one more interesting result. After replacing r L in the 3 8 considered acoustic near ﬁeld, Lighthill’s power law gives the scaling [1,5] jIj r c (j~vj/c ) . If we 0 0 further ignore the multiplication constant which is determined by the dimensionless k, this matches Equation (29) if we set 2 2 c L c 0 0 G = , (30) 2M 2r L where M is total mass of the source. In this way we can identify length scale of the source L as the acoustic Schwarzschild radius, 2GM L = . (31) In cosmology, Schwarzschild radius determines length scale of a source of gravitational waves, such as a rotating black hole in a black-hole binary. The same concept appears to characterize length scale of the source of waves in the analogue acoustic spacetime. It is worth mentioning that compact sources of longitudinal waves are much less efﬁcient than sources of transverse waves. The reason is that the second-order time derivative in Equations (17) 2 4 and (20) leaves the multiplication factor (wL/c ) in the expression for wave amplitude and (wL/c ) 0 0 for radiated power, with wL/c 1. In fact, the weak longitudinal component is completely removed in the transverse-traceless gauge, which is typically used for transverse gravitational waves in the linearized theory. However, the ﬂuids do not support propagation of transverse acoustic waves and the remaining longitudinal waves obey the eighth power law. 4. Conclusions Although Lighthill’s power law for a quadrupole source in an inviscid incompressible ﬂow is merely reproduced using the formalism of the acoustic spacetime analogy, the derivation given above has several important implications. First, the description of sound generation in acoustic spacetime appears to be more natural than the classical derivation based on the conservation laws. The entire stress–energy tensor is taken as the source of waves, without splitting it into the source and propagation terms or selecting an appropriate dynamic quantity (acoustic pressure or density) for the aeroacoustic analogy. Second, generated sound waves are treated as a purely geometric perturbation of the background acoustic spacetime, described by the weak unsteady component of the metric tensor. Rather than contracting the second-order tensor in the source term with double divergence, the entire metric tensor ﬁeld associated with sound waves is observed and the acoustic scalar component is extracted by the choice of Newtonian gauge. Third, the derivation of the eighth power law proves that the acoustic spacetime analogy can be extended beyond sound propagation to aeroacoustic sound generation, at least in incompressible ﬂows where the kinematic effects dominate. Hence, the acoustic analogy covers not only the background metric, but the sound waves and kinematic sources, as well. Acoustics 2020, 2 673 The applied methodology can include sound propagation effects in a non-uniform ﬂow outside ab the source region, such as convection and refraction. The Minkowski metric h in Equation (3) should be replaced accordingly with an appropriate background metric [10]. These effects cannot be retrieved from the analogy with gravitation, since curvature of the background acoustic spacetime depends on the state of the external steady ﬂow, not mass itself. The acoustic analogy indeed captures kinematics and not dynamics of general relativity. However, this does not imply that the Einstein ﬁeld equations with the source term cannot be used for capturing unsteady changes of the acoustic spacetime, as demonstrated above. This is possible exactly because sound generation in an incompressible ﬂow is purely kinematic and the stress–energy tensor reduces to the same form in both theories for non-relativistic velocities. The analysis was based on the linearized theory of weak perturbation and free-space sound generation in low Mach number ﬂows. Further investigation is necessary in order to check whether the analogy can be extended to include certain non-linear acoustic phenomena and high Mach number ﬂows, or the effects of boundaries in the ﬂow, such as reduction of aeroacoustic quadrupole to dipole, although in such case the analogy with covariant electromagnetism appears to be more natural. The obtained results also open the possibilities for further studies of the analogy between vortex pairs, as compact aeroacoustic sources, and rotating black-hole binaries, as typical sources of gravitational waves. Author Contributions: Conceptualization, D.M.; methodology, D.M.; validation, E.S.; writing—original draft preparation, D.M.; supervision, E.S. All authors have read and agreed to the published version of the manuscript. Funding: This research received no external funding. Conﬂicts of Interest: The authors declare no conﬂict of interest. References 1. Lighthill, M.J. On sound generated aerodynamically, I. General theory. Proc. R. Soc. Lond. 1952, A211, 564–586. 2. Schutz, B. A First Course in General Relativity, 2nd ed.; Sections 8 and 9; Cambridge University Press: Cambridge, UK, 2017. 3. Gordon, W. Zur Lichtfortpﬂanzung nach der Relativitätstheorie (“Towards propagation of light based on the theory of relativity”). Ann. Phys. 1923, 72, 421–456. [CrossRef] 4. Jones, D.S. Acoustic and Electromagnetic Waves; Oxford University Press: Oxford, UK, 1986; pp. 10–14. 5. Rienstra, S.W.; Hirschberg, A. An Introduction to Acoustics; Sections 6.5 and 9.1; Eindhoven University of Technology: Eindhoven, The Netherlands, 2018. 6. Unruh, W.G. Experimental black-hole evaporation. Phys. Rev. Lett. 1981, 46, 1351–1353. [CrossRef] 7. Barceló, C.; Liberati, S.; Visser, M. Analogue gravity. Living Rev. Relativ. 2011, 14, 1–151. [CrossRef] [PubMed] 8. Barceló, C.; Liberati, S.; Sonego, S.; Visser, M. Causal structure of analogue spacetimes. New J. Phys. 2004, 6, 1–48. [CrossRef] 9. Pierce, A.D. Wave equation for sound in ﬂuids with unsteady inhomogeneous ﬂow. J. Acoust. Soc. Am. 1990, 87, 2292–2299. [CrossRef] 10. Gregory, A.; Agarwal, A.; Lasenby, J.; Sinayoko, S. Geometric algebra and an acoustic space time for propagation in non-uniform ﬂow. In Proceedings of the 22nd International Congress on Sound and Vibration (ICSV), Florence, Italy, 12–16 July 2015. 11. Bergliaffa, S.E.P.; Hibberd, K.; Stone, M.; Visser, M. Wave equation for sound in ﬂuids with vorticity. Physica D 2004, 191, 121–136. [CrossRef] 12. Misner, C.W.; Thorne, K.S.; Wheeler, J.A. Gravitation; Sections 35 and 36; Princeton University Press: Princeton, NJ, USA, 2017. c 2020 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license (http://creativecommons.org/licenses/by/4.0/).

Acoustics – Multidisciplinary Digital Publishing Institute

**Published: ** Sep 8, 2020

**Keywords: **acoustic spacetime; Lighthill’s aeroacoustic analogy; quadrupole radiation

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