Probing a more stable part of scattered disk as a source of Jupiter-family comets

We study the origin of the Jupiter-family comets. We focus our attention on the part of the scattered disk where the perihelion distance is in the interval from 35 to 40 AU, considering this region as a source, from which the comets start their migration to the Jupiter family. To be more specific, we perform a numerical simulation of the dynamical evolution of 5179 massless test particles, which represent the objects in the scattered disk. The simulation maps the routes of the transit from the orbital phase-space of the scattered disk to that of the Jupiter-family comets. We predict the dynamical structure of this population. Some predicted dynamical properties of the group are compared with the observed Jupiter-family comets.