Abstract
We discuss the dynamical formation of small Solar System objects beyond Neptune. The discovery of the first trans-Neptunian object (TNO) - except for Pluto and Charon - is relatively recent (1992QB_1). Many unpredicted dynamical and physical features not predicted in past theoretical models and are now showing up. Among them, we note the existence of many high-inclined orbits with respect to the eclipitc plane (where all Solar System bodies supposedly have formed). The aim of this work is to show a dynamical pathway from the primordial planetesimal disk to high inclinations orbits in the trans-Neptunian region. The main mechanism requires that scattered planetesimals are captured into some exterior mean motion resonance (MMR) with Neptune and then be trapped into the Kozai resonance as well. After that, some planetesimals may access a resonance hibernating mode in which the planesimal is barely locked in resonance. We show that only a few percent of all scattered planetesimals would access the hibernating mode. But, once this mechanism is active, ∼ 100% of the particles would escape both resonances while Neptune is in its final migration stage (after the LHB phase). Our results could explain at least a portion (up to 80%) of the classical hot population, defined by a_{2:3}<a<a_{1:2}, i>5^{o}, and q>36au. Previous results indicate that this mechanism is the most likely to form the detached objects close to MMR with Neptune as, for example, 2004XR_{190} (Gomes, 2011, Icarus 215, 661). We have determined the most probable regions, in the orbital elements space (a, e, i), where detached objects would form close to 2:5 and 1:3 MMRs (Brasil, Gomes & Soares, 2013 - submitted to A&A).
