Effect of the planetesimal disk on the positions of the secular resonances
Résumé
During the pre-instability period following the disappearance of the protoplanetary gas disk, the giant planets were in a compact multiresonant orbital configuration, before starting to migrate by interacting with the planetesimal disk extending beyond the orbit of Neptune. It is commonly accepted that the planetesimal disk was divided into two parts: a massive disk extending from Neptune to 30 au and a low mass extension of the disk, extending beyond 30 au. We study the effect of the massive part of the disk on the nodal precessions of the giant planets and of the planetesimals in order to find the positions of the nodal secular resonances. The presence of the massive disk removes the degeneracy of the f_{5} nodal frequency and allows for a new secular resonance. We show that for some orbital configurations, the f_{5} nodal secular resonance is located in the region where the primordial cold classical Kuiper Belt formed.