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R.S. Gomes (GEA/OV/MCT & ON/MCT)
I present the results of a numerical integration extending to the age of the Solar System, starting with the major planets at initial compact orbits and a disk of planetesimals with its inner edge just outside the outermost planet and its outer edge at around 30 AU. These planetesimals perturb the planets but not themselves. In the end of the integration, some high inclination objects are deposited into the classical Kuiper Belt (between the 2:3 and 1:2 resonance with Neptune). Other scattered objects acquire relatively high perihelia beyond the 1:2 resonance, thus forming the extended scattered population. Finally, some other objects are placed in the 2:3 resonance (Plutinos) and other mean motion resonances. The formation of the classical objects is associated to secular resonances whereas the extended scattered objects acquire relatively low eccentricities due to the action of high order mean motion resonances with Neptune associated to the Kozai resonance. High inclination resonant TNO's mostly come from the original scattered population although some may be a result of the resonance sweeping mechanism by the primordial migrating Neptune. Finally, I present a comparison with the real high inclination TNO population.
The author(s) of this abstract have provided an email address for comments about the abstract: rodney@ov.ufrj.br
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Bulletin of the American Astronomical Society, 36 #2
© 2004. The American Astronomical Soceity.