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We explore the dynamical evolution of a planet embedded in a disk surroundinga star part of a binary system where the orbital plane of the binary issignificantly tilted respect to the initial disk plane. Our aim is to testwhether the planet remains within the disk and continues to migrate towards thestar in a Type I/II mode in spite of the secular perturbations of the companionstar. This would explain observed exoplanets with significant inclinationrespect to the equatorial plane of their host star. We have used two differentSPH codes, vine and phantom, to model the evolution of a systemstar+disk+planet and companion star with time. After an initial coupledevolution, the inclination of the disk and that of the planet begin to differsignificantly. The period of oscillation of the disk inclination, respect tothe initial plane, is shorter than that of the planet which evolvesindependently after about 10^4 yr following a perturbed N-body behavior.However, the planet keeps migrating towards the star because during its orbitalmotion it crosses the disk plane and the friction with the gas causes angularmomentum loss. Disk and planet in a significantly inclined binary system arenot dynamically coupled for small binary separations but evolve almostindependently. The planet abandons the disk and, due to the onset of asignificant mutual inclination, it interacts with the gas only when its orbitintersects the disk plane. The drift of the planet towards the star is not dueto type I/II with the planet embedded in the disk but to the friction with thegas during the disk crossing.

Decoupling of a giant planet from its disk in an inclined binary system