  We explore the dynamical evolution of a planet embedded in a disk surrounding
a star part of a binary system where the orbital plane of the binary is
significantly tilted respect to the initial disk plane. Our aim is to test
whether the planet remains within the disk and continues to migrate towards the
star in a Type I/II mode in spite of the secular perturbations of the companion
star. This would explain observed exoplanets with significant inclination
respect to the equatorial plane of their host star. We have used two different
SPH codes, vine and phantom, to model the evolution of a system
star+disk+planet and companion star with time. After an initial coupled
evolution, the inclination of the disk and that of the planet begin to differ
significantly. The period of oscillation of the disk inclination, respect to
the initial plane, is shorter than that of the planet which evolves
independently after about 10^4 yr following a perturbed N-body behavior.
However, the planet keeps migrating towards the star because during its orbital
motion it crosses the disk plane and the friction with the gas causes angular
momentum loss. Disk and planet in a significantly inclined binary system are
not dynamically coupled for small binary separations but evolve almost
independently. The planet abandons the disk and, due to the onset of a
significant mutual inclination, it interacts with the gas only when its orbit
intersects the disk plane. The drift of the planet towards the star is not due
to type I/II with the planet embedded in the disk but to the friction with the
gas during the disk crossing.
