  Planet Planet scattering is a leading dynamical mechanism invoked to explain
the present orbital distribution of exoplanets. Many stars belong to binary
systems, therefore it is important to understand how this mechanism works in
presence of a companion star. We focus on systems of three planets orbiting the
primary star and estimate the timescale for instability finding that it scales
with the keplerian period for systems that have the same ratio between inner
planet and binary semimajor axes. An empirical formula is also derived from
simulations to estimate how the the binary eccentricity affects the extent of
the stability region. The presence of the secondary star affects the Planet
Planet scattering outcomes causing a broadening of the final distribution in
semimajor axis of the inner planet as some of the orbital energy of the planets
is absorbed by the companion star. Repeated approaches to the secondary star
causes also a significant reduction in the frequency of surviving two planet
systems in particular for larger values of the inner planet semimajor axis. The
formation of Kozai states with the companion star increases the number of
planets which may be tidally circularized. To predict the possible final
distribution of planets in binaries we have performed a large number of
simulations where the initial semimajor axis of the inner planets is chosen
randomly. For small values of the binary semimajor axis, the higher frequency
of collision alter the final planet orbital distributions which, however,
beyond 50 au appear to be scalable to wider binary separations.
