Energy Density, Energy Flux and Momentum Flux of Surface Waves
[math]\displaystyle{ \varepsilon(t) = \ \mbox{Energy in control volume} \ \gamma(t) }[/math] :
[math]\displaystyle{ \varepsilon (t) = \rho \iiint_V \left( \frac{1}{2} V^2 + gZ \right) dV }[/math]
Mean energy over unit horizongtal surface area [math]\displaystyle{ S \, }[/math] :
[math]\displaystyle{ \overline{\varepsilon} = \overline{\frac{\varepsilon(t)}{S}} = \rho \overline{ \int_{-H}^{\zeta(t)} \left( \frac{1}{2} V^2 + gZ \right) dZ} = \frac{1}{2} \rho \overline{ \int_{-H}^{\zeta(t)} V^2 dZ} + \overline{ \frac{1}{2} \rho g ( \zeta^2 - H^2 ) } }[/math]
where [math]\displaystyle{ \zeta(t) \, }[/math] is free surface elevation.
Ignore term [math]\displaystyle{ -\frac{1}{2} \rho g H^2 \, }[/math] which represents the potential energy of the ocean at rest.
The remaining perturbation component is the sum of the kinetic and potential energy components
[math]\displaystyle{ \overline{\varepsilon} = \overline{\varepsilon_{kin}} + \overline{\varepsilon_{pot}} }[/math]
[math]\displaystyle{ \overline{\varepsilon_{kin}} = \frac{1}{2} \rho \overline{\int_{-H}^{\zeta(t)} V^2 dZ}, \qquad V^2 = \nabla\Phi \cdot \nabla \Phi = \Phi_X^2 + \Phi_Z^2 }[/math]
[math]\displaystyle{ \overline{\varepsilon_{pot}} = \overline{\frac{1}{2} \rho g \zeta^2 (t)} }[/math]
Consider now as a special case plane progressive waves defined by the velocity potential in deep water (for simplicity):
[math]\displaystyle{ \Phi = \mathbf{Re} \{ \frac{igA}{\omega} e^{KZ-iKX+i\omega t} \} }[/math]
[math]\displaystyle{ \Phi_X = \mathbf{Re} \{ \frac{igA}{\omega} (-iK) e^{KZ-iKX+i\omega t} \} }[/math]
[math]\displaystyle{ = A \mathbf{Re} \{ \omega e^{KZ-iKX+i\omega t} \} }[/math]
[math]\displaystyle{ \Phi_Z = \mathbf{Re} \{ \frac{iSA}{\omega} K e^{KZ-iKX+i\omega t} \} }[/math]
[math]\displaystyle{ = A \mathbf{Re} \{ i \omega e^{KZ-iKX+i\omega t} \} }[/math]
Lemma
Let:
[math]\displaystyle{ \mathbf{Re} \{ A e^{i\omega t} \} = A(t) }[/math]
[math]\displaystyle{ \mathbf{Re} \{ B e^{i\omega t} \} = B(t) }[/math]
[math]\displaystyle{ \overline{A(t)B(t)} = \frac{1}{2} \mathbf{Re} \{ A B^* \} }[/math]
[math]\displaystyle{ \overline{\epsilon_{kin}} = \frac{1}{2} \rho \overline{ ( \int_{-\infty}^0 + \int_0^\zeta ) \left( \Phi_X^2 + \Phi_Z^2 \right) } dZ }[/math]
[math]\displaystyle{ = \frac{1}{2} \rho \int_{-\infty}^0 \left( \Phi_X^2 + \Phi_Z^2 \right) dZ + O (A^3) }[/math]
[math]\displaystyle{ = \rho \frac{\omega^2 A^2}{4K} = \frac{1}{4} \rho g A^2 , \qquad \mbox{for} \ K=\omega^2/g }[/math]
[math]\displaystyle{ \overline{\varepsilon_{pot}} = \frac{1}{2} \rho g {\overline{\zeta(t)}}^2 = \frac{1}{4} \rho g A^2 }[/math]
Hence:
[math]\displaystyle{ \overline{\varepsilon} = \overline{\varepsilon_{kin}} + \overline{\varepsilon_{pot}} = \frac{1}{2} \rho g A^2 }[/math]
Energy flux = rate of change of energy density [math]\displaystyle{ \varepsilon(t) }[/math]
[math]\displaystyle{ P(t) \equiv \frac{d\varepsilon(t)}{dt} , \ \varepsilon = \iiint_V(t) (\frac{1}{2} \rho V^2 +gZ ) d }[/math]
[math]\displaystyle{ P(t) = \frac{d \varepsilon(t)}{dt} = \frac{d}{dt} \iiint_V(t) \epsilon(t) dV = \iint_S(t) \frac{\partial \epsilon(t)}{\partial t} dV + \iint_S(t) \epsilon(t) U_n dS }[/math]
Transport theorem where [math]\displaystyle{ U_n }[/math] is normal velocity of surface [math]\displaystyle{ S(t) }[/math] outwards of the enclosed volume [math]\displaystyle{ V }[/math].
[math]\displaystyle{ \frac{\partial \epsilon}{\partial t} = \frac{\partial}{\partial t} \{ \frac{1}{2} \rho V^2 + \rho g Z \} = \frac{1}{2} \rho \frac{\partial}{\partial t} ( \nabla\Phi \cdot \nabla\Phi) }[/math]
[math]\displaystyle{ = \rho \nabla \cdot \left( \frac{\partial\Phi}{\partial t} \nabla\Phi \right) - \rho \frac{\partial\Phi}{\partial t} \nabla^2 \Phi }[/math]
[math]\displaystyle{ P(t) = \frac{d \varepsilon(t)}{dt} = \rho \iiint_V(t) \nabla \cdot \left( \frac{\partial \Phi}{\partial t} \nabla \Phi \right) dV + \rho \iint_S(t) \left( \frac{1}{2} V^2 + gZ \right) U_n dS }[/math]
Invoking the scalar form of Gauss's theorem in the frist term, we obtain:
[math]\displaystyle{ P(t) = \rho \iint \frac{\partial\Phi}{\partial t} \nabla \Phi \dot \vec n ds + \rho \iint \left( \frac{1}{2} V^2 + gZ \right) U_n ds }[/math]
An alternative form for the energy flux [math]\displaystyle{ P(t) \, }[/math] crossing the closed control surface [math]\displaystyle{ S(t) \, }[/math] is obtained by invoking Bernoulli's equation in the second term. Recall that:
[math]\displaystyle{ \frac{P-P_a}{\rho} + \frac{\partial\Phi}{\partial t} + \frac{1}{2} \nabla\Phi \dot \nabla\Phi + gZ = 0 }[/math]
At any point in the fluid domain and on boundarie.
Here we did allow [math]\displaystyle{ \ P_a \equiv \mbox{Atmospheric pressure} \ }[/math] to be non-zero for the sake of physical clarity. Upon substitution in [math]\displaystyle{ P(t) }[/math] we obtain the alternate form:
[math]\displaystyle{ P(t) = \rho \iint \frac{\partial\Phi}{\partial t} \frac{\partial\Phi}{\partial n} ds - \rho \iint \left( \frac{P-P_a}{\rho} + \frac{\partial\Phi}{\partial t} \right) U_n ds }[/math]
So the energy flux across [math]\displaystyle{ S(t)\, }[/math] is given by the terms under the interral sign. They can be collected in the more compact form:
[math]\displaystyle{ P(t) = \iint \left\{ \rho \frac{\partial\Phi}{\partial t} \left( \frac{\partial\Phi}{\partial n} - U_n \right) - ( P - P_a) U_n \right\} ds }[/math]
Note that [math]\displaystyle{ P(t) \, }[/math] measures the energy flux into the volume [math]\displaystyle{ V(t) \, }[/math] or the rate of growth of the energy density [math]\displaystyle{ \varepsilon(t)\, }[/math].
We are ready now to apply the above formulae to the surface wave propagation problem.
Break [math]\displaystyle{ S(t) \, }[/math] into tis components and derive specialized forms of [math]\displaystyle{ P(t) \, }[/math] pertinent to each.
[math]\displaystyle{ S_F : \ \mbox{nonlinear position of the free surface} }[/math]
[math]\displaystyle{ \frac{\partial\Phi}{\partial n} = U_n; \ \mbox{normal flow velocity} \equiv \mbox{normal velocity of free surface boundary; kinematic condition}. }[/math]
[math]\displaystyle{ P = P_a; \ \mbox{fluid pressure} \equiv \mbox{atmospheric} }[/math]
Therefore over [math]\displaystyle{ S_F; \ P(t) \equiv 0 }[/math] as expected. No energy can flow into the atmosphere!
[math]\displaystyle{ S_B: \ \mbox{non-moving solid boundary} }[/math]
[math]\displaystyle{ U_n = 0, \ \frac{\partial\Phi}{\partial n} = U_n; \ \mbox{no-normal flux condition} }[/math]
[math]\displaystyle{ S^\pm: \ \mbox{fluid boundaries fixed in space relative to an earth frame} }[/math]
[math]\displaystyle{ U_n = 0, \ \frac{\partial\Phi}{\partial n} \ne 0 }[/math]
[math]\displaystyle{ S_U: \ \mbox{fluid boundaries moving w. velocity} \ \vec{U} \ \mbox{relative to an earth frame} }[/math]
[math]\displaystyle{ U_n = \vec U \cdot \vec n, \quad \frac{\partial\Phi}{\partial n} \ne 0 }[/math]
This case will be of interest later in the course when we consider ships moving with constant velocity [math]\displaystyle{ U }[/math].
The formulae derived above are very general for potential flows with a free surface and solid boundaries. We are now ready to apply them to plane progressive waves.
Energy flux across a vertical fluid boundary fixed in space.
[math]\displaystyle{ \frac{P(t)}{\mbox{width}} = - \rho \int_{-infty}{\zeta(t)} \frac{\partial\Phi}{\partial t} \Phi_n dZ = - \rho \left( \int_{-\infty}^0 + \int_0^\zeta \right) \frac{\partial\Phi}{\partial t} \Phi_n dZ = - \rho \int_{-infty}^0 \frac{\partial\Phi}{\partial t} \frac{\partial\Phi}{\partial n} dZ + O(A^3) }[/math]
