  This paper examines the energetics of a convective flow subject to an
oscillation with a period $t_{\rm osc}$ much smaller than the convective
timescale $t_{\rm conv}$, allowing for compressibility and uniform rotation. We
show that the energy of the oscillation is exchanged with the kinetic energy of
the convective flow at a rate $D_R$ that couples the Reynolds stress of the
oscillation with the convective velocity gradient. For the equilibrium tide and
inertial waves, this is the only energy exchange term, whereas for p modes
there are also exchanges with the potential and internal energy of the
convective flow. Locally, $\left| D_R \right| \sim u^{\prime 2} /t_{\rm conv}$,
where $u^{\prime}$ is the oscillating velocity. If $t_{\rm conv} \ll t_{\rm
osc}$ and assuming mixing length theory, $\left| D_R \right|$ is $\left(
\lambda_{\rm conv}/ \lambda_{\rm osc} \right)^2$ smaller, where $\lambda_{\rm
conv}$ and $\lambda_{\rm osc}$ are the characteristic scales of convection and
the oscillation. Assuming local dissipation, we show that the equilibrium tide
lags behind the tidal potential by a phase $\delta \left( r \right) \sim r
\omega_{\rm osc}/ \left( g \left( r \right) t_{\rm conv} \left( r
\right)\right)$, where $g$ is the gravitational acceleration. The equilibrium
tide can be described locally as a harmonic oscillator with natural frequency
$\left( g / r \right)^{1/2}$ and subject to a damping force $-u^{\prime}/t_{\rm
conv}$. Although $\delta \left( r \right) $ varies by orders of magnitude
through the flow, it is possible to define an average phase shift
$\overline{\delta}$ which is in good agreement with observations for Jupiter
and some of the moons of Saturn. Finally, $1 / \overline{\delta}$ is shown to
be equal to the standard tidal dissipation factor.
