  The satellite Mimas launches a bending wave -- a warping of the rings that
propagates radially through self-gravity -- at the 5:3 inner vertical resonance
with Saturn's rings. We present a modification of the linear bending wave
theory which includes the effects of satellite self-gravity wakes on the
particles in the wave. We show that, when treated as rigid, these wakes
generate an extra layer of particles whose number density is proportional to
the magnitude of the slope of the warped ring. Using a ray-tracing code we
compare our predictions with those of linear bending wave theory and with 60
stellar occultations observed by the Cassini Ultraviolet Imaging Spectrograph
(UVIS) and find that the extra layer of particles of our perturbed bending wave
model has a considerable explanatory power for the UVIS dataset. Our best model
explains the most discrepant and surprising features of the Mimas 5:3 bending
wave; the enhancement of the signal for the cases of occultations with high
ring opening angle and the bigger-than-expected viscosity, $\nu = 576 \,
\mathrm{cm^2/s}$, which is more than double the viscosity computed from density
waves. This shows that self-gravity wakes can be effective at transporting
angular momentum in a vertically perturbed disk. Relative to neighboring
density waves, we find a lower-than-expected value for the surface mass
density, $\sigma = 36.7 \, \mathrm{g/cm^2}$, which suggests that the enhanced
viscous interactions may be transporting material into the surrounding regions.
