  Saturns F-ring is a unique, narrow ring that lies (radially) close to the
tidally disruptive Roche limit of water ice for Saturn. Significant work has
been done that shows it to be one of the most dynamic places in the Solar
System. Aggregates that are fortunate enough to form constantly battle against
the strong tidal forces of Saturn and the nearby moons Prometheus and Pandora,
which act to gravitationally stir up ring material. Planetary rings are also
known to radially spread. Therefore, as the F ring lies at the edge of the main
rings, we investigate the effect of an outwardly migrated F ring and its
interaction with Prometheus. An increase in the maximum number density of
particles at the channel edges is observed with decreasing local tidal
environment. Radial velocity dispersions are also observed to fall below the
typical escape velocity of a 150m icy moonlet (<10 cm s^(-1)) where density is
enhanced, and are gravitationally unstable with Toomre parameters Q<2.
Additionally, in locations of the ring where Q<2 is observed, more particles
are seen to fall below or close to the critical Toomre parameter as the radial
location of the ring increases.
