  With n-body simulations, we model terrestrial circumbinary planet (CBP)
formation with an initial surface density profile motivated by hydrodynamic
circumbinary gas disc simulations. The binary plays an important role in
shaping the initial distribution of bodies. After the gas disc has dissipated,
the torque from the binary speeds up the planet formation process by promoting
body-body interactions but also drives the ejection of planet building material
from the system at an early time. Fewer but more massive planets form around a
close binary compared to a single star system. A sufficiently wide or eccentric
binary can prohibit terrestrial planet formation. Eccentric binaries and
exterior giant planets exacerbate these effects as they both reduce the radial
range of the stable orbits. However, with a large enough stable region, the
planets that do form are more massive, more eccentric and more inclined. The
giant planets remain on stable orbits in all our simulations suggesting that
giant planets are long-lived in planetary systems once they are formed.
