  Star clusters that form in nuclear rings appear to be at slightly larger
radii than the gas. We argue that the star clusters move out from the gas in
which they are formed because of satellite-disk tidal interactions. In
calculating the dynamics of this star cluster and gas ring system, we include
the effects of dynamical friction of the background stars in the host galaxy on
the star cluster, and inflowing gas along the bar onto the nuclear ring at the
two contact points. We show that the final separation is of the order of the
Hill radius of the nuclear ring, which is typically 20-30% of its radius.
Massive star clusters can reach half of this separation very quickly and
produce a factor of a few enhancement in the gas surface density. If this leads
to star formation in addition to the (ongoing) formation of star clusters near
the contact points, a possible (initial) azimuthal age gradient may become
diluted or even disappear. Finally, if the star cluster are massive and/or
numerous enough, we expect the nuclear ring to migrate inward, away from the
(possibly) associated (inner) Lindblad resonance. We discuss how these
predictions may be tested observationally.
