  Saturn's C ring contains multiple spiral patterns that appear to be density
waves driven by periodic gravitational perturbations. In other parts of
Saturn's rings, such waves are generated by Lindblad resonances with Saturn's
various moons, but most of the wave-like C-ring features are not situated near
any strong resonance with any known moon. Using stellar occultation data
obtained by the Visual and Infrared Mapping Spectrometer (VIMS) onboard the
Cassini spacecraft, we investigate the origin of six unidentified C-ring waves
located between 80,900 and 87,200 km from Saturn's center. By measuring
differences in the waves' phases among the different occultations, we are able
to determine both the number of arms in each spiral pattern and the speeds at
which these patterns rotate around the planet. We find that all six of these
waves have between 2 and 4 arms and pattern speeds between 1660 degrees/day and
1861 degrees/day. These speeds are too large to be attributed to any satellite
resonance. Instead they are comparable to the predicted pattern speeds of waves
generated by low-order normal-mode oscillations within the planet [Marley &
Porco 1993, Icarus 106, 508]. The precise pattern speeds associated with these
waves should therefore provide strong constraints on Saturn's internal
structure. Furthermore, we identify multiple waves with the same number of arms
and very similar pattern speeds, indicating that multiple m=3 and m=2 sectoral
(l=m) modes may exist within the planet.
