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Internal Wave Generation in Uniformly Stratified Fluids. 1 ... - LEGI

Internal Wave Generation in Uniformly Stratified Fluids. 1 ... - LEGI

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particles move as expected along radial trajectories. Out of the characteristic cone the pressure<br />

and velocity are π/2 out of phase imply<strong>in</strong>g that no energy flux, proportional to Re [Pv *] where<br />

* denotes a complex conjugate (see Lighthill 1978 § 4.2), is radiated. Energy, and thus<br />

<strong>in</strong>ternal waves, are conf<strong>in</strong>ed on the cone, where they diverge. There, po<strong>in</strong>t sources are no<br />

more an adequate model of real sources of <strong>in</strong>ternal waves. Only the consideration of the f<strong>in</strong>ite<br />

extent of the latter will account for the radial decrease as 1/√r, and the transverse phase<br />

variations, experimentally exhibited by McLaren et al. (1973).<br />

7.2. Bouss<strong>in</strong>esq impulsive waves<br />

Pass<strong>in</strong>g to impulsive <strong>in</strong>ternal waves we commence as <strong>in</strong> § 6.1 by study<strong>in</strong>g the<br />

Bouss<strong>in</strong>esq pressure and velocity fields. For small times Nt « 1, either differentiat<strong>in</strong>g (6.7)<br />

accord<strong>in</strong>g to (3.11)-(3.12) or asymptotically <strong>in</strong>vert<strong>in</strong>g (7.3)-(7.4) by (D1), we obta<strong>in</strong><br />

PB(r, t) ~ ρ0m0<br />

4πr<br />

vB(r, t) ~ m0<br />

4πr 2 r r<br />

δ'(t) , (7.5)<br />

δ(t) . (7.6)<br />

The pressure and velocity impulses necessary to set the fluid <strong>in</strong>to motion are recovered (cf.<br />

appendix B).<br />

In similarly differentiat<strong>in</strong>g the expansion of the Green’s function for large times Nt » 1,<br />

care must be taken to reta<strong>in</strong> the first two orders of (6.8) and (6.10) so as to recover the<br />

presence of buoyancy oscillations. Lighthill’s (1958) method may also be applied to (7.3)-<br />

(7.4), <strong>in</strong> which cases it <strong>in</strong>volves (D3)-(D4). Both procedures yield<br />

PB(r, t) ~ – H(t) ρ0 N 2 m0<br />

2π 3/2 r<br />

vB(r, t) ~ – H(t) Nm0<br />

2π 3/2 r 2 r r<br />

s<strong>in</strong> θ cos θ s<strong>in</strong> Nt cos θ – π/4<br />

Nt cos θ<br />

– 1<br />

s<strong>in</strong> θ<br />

s<strong>in</strong> θ Nt cos θ s<strong>in</strong> Nt cos θ – π/4 + 1<br />

s<strong>in</strong> 3 θ<br />

s<strong>in</strong> Nt – π/4<br />

Nt 3/2<br />

cos Nt – π/4<br />

Nt 3/2<br />

, (7.7)<br />

.<br />

(7.8)<br />

The phase Φ g = Nt⏐cos θ⏐ – π/4 of gravity waves is, apart from a phase lag of π/4,<br />

identical to that deduced from the consideration of group velocity. Thus, gravity waves<br />

propagate as the locally plane waves described <strong>in</strong> § 4.1, with the group velocity c g = r/t and<br />

the frequency and wavevector<br />

<strong>Internal</strong> wave generation. 1. Green’s function 29

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