  The Pluto-Charon system has come into sharper focus following the fly by of
New Horizons. We use N-body simulations to probe the unique dynamical history
of this binary dwarf planet system. We follow the evolution of the debris disc
that might have formed during the Charon-forming giant impact. First, we note
that in-situ formation of the four circumbinary moons is extremely difficult if
Charon undergoes eccentric tidal evolution. We track collisions of disc debris
with Charon, estimating that hundreds to hundreds of thousands of visible
craters might arise from 0.3--5 km radius bodies. New Horizons data suggesting
a dearth of these small craters may place constraints on the disc properties.
While tidal heating will erase some of the cratering history, both tidal and
radiogenic heating may also make it possible to differentiate disc debris
craters from Kuiper belt object craters. We also track the debris ejected from
the Pluto-Charon system into the Solar System; while most of this debris is
ultimately lost from the Solar System, a few tens of 10--30 km radius bodies
could survive as a Pluto-Charon collisional family. Most are plutinos in the
3:2 resonance with Neptune, while a small number populate nearby resonances. We
show that migration of the giant planets early in the Solar System's history
would not destroy this collisional family. Finally, we suggest that
identification of such a family would likely need to be based on composition as
they show minimal clustering in relevant orbital parameters.
