  Transiting circumbinary planets discovered by Kepler provide unique insight
into binary star and planet formation. Several features of this new found
population, for example the apparent pile-up of planets near the innermost
stable orbit, may distinguish between formation theories. In this work, we
determine how planet-planet scattering shapes planetary systems around binaries
as compared to single stars. In particular, we look for signatures that arise
due to differences in dynamical evolution in binary systems. We carry out a
parameter study of N-body scattering simulations for four distinct planet
populations around both binary and single stars. While binarity has little
influence on the final system multiplicity or orbital distribution, the
presence of a binary dramatically effects the means by which planets are lost
from the system. Most circumbinary planets are lost due to ejections rather
than planet-planet or planet-star collisions. The most massive planet in the
system tends to control the evolution. Systems similar to the only observed
multi-planet circumbinary system, Kepler-47, can arise from much more tightly
packed, unstable systems. Only extreme initial conditions introduce differences
in the final planet populations. Thus, we suggest that any intrinsic
differences in the populations are imprinted by formation.

Earth and Planetary Astrophysics;Solar and Stellar Astrophysics