  The aim of this work is to study the impact of a binary companion on the
evolution of two-planet systems during both the type-II migration phase and
their long-term evolution after the dissipation of the protoplanetary disk. We
use the symplectic integrator SyMBA, modified to include a wide binary
companion. We also include the Type-II migration of giant planets during the
disk phase with suitable eccentricity and inclination damping as well as the
disk gravitational potential acting on the planets and the nodal precession of
the disk induced by the binary companion. We consider various inclinations,
eccentricities, and separations of the binary companion. Disk migration allows
the formation of planet pairs in mean-motion resonances (MMR) despite the
presence of the binary companion. When the binary separation is wide (1000au),
the timescale of the perturbations it raises on the planets is longer than the
disk's lifetime and resonant pairs are routinely formed in the 2:1, 5:2 and 3:1
MMR. Provided the planet-planet interaction timescale is smaller than the
binary perturbations timescale, these systems can remain in resonance long
after the disk has dissipated. When the binary separation is smaller (250au),
only planets in the 2:1 resonance tend to remain in a resonant state and more
chaotic evolutions are observed, as well as more ejections. After those
ejections, the remaining planet can become eccentric due to the perturbations
from the binary companion and for strongly inclined binary companions captures
in the von Ziepel-Lidov-Kozai resonance can occur, while in systems with two
planets this mechanism is quenched by planet-planet interactions. Our
simulations reveal that the interplay between planet-disk, planet-planet and
planet-binary interactions can lead to the formation of resonant pairs of
planets which remain stable over timescales much longer than the disk's
lifetime.
