  Tidal dissipation inside giant planets is important for the orbital evolution
of their natural satellites. It is conventionally treated by parameterized
equilibrium tidal theory, in which the tidal torque declines rapidly with
distance, and orbital expansion was faster in the past. However, Lainey et al.
(2017) find that some Saturnian satellites are currently migrating outward
faster than predicted by equilibrium tidal theory. Resonance locking between
satellites and internal oscillations of Saturn, proposed by Fuller et al.
(2016), naturally matches the observed migration rates. Here, we show that the
resonance locking theory predicts dynamical tidal perturbations to Saturn's
gravitational field in addition to those produced by equilibrium tidal bulges.
We show that these perturbations can likely be detected during Cassini's
proximal orbits if migration of satellites results from resonant gravity modes,
but will likely be undetectable if migration results from inertial wave
attractors or dissipation of the equilibrium tide. Additionally, we show that
the detection of gravity modes would place constraints on the size of the
hypothetical stably stratified region in Saturn.
