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N. Callegari Jr. (IAG-USP), T. A. Michtchenko, S. Ferraz-Mello (IAG-USP)
The dynamics of two planets near first order mean motion resonances is modeled in the domain of the general three-body planar problem. The systems studied are the pair Uranus-Neptune (2:1 resonance) and planets B-C of the pulsar PSR B1257+12 (3:2). The phase space in the resonance and near-resonance regions is studied by means of surfaces of section and spectral map techniques. After a thorough investigation of the topology of the phase spaces, we find that several regimes of motion are possible for both Uranus-Neptune and B-C planetary systems. Moreover, when the masses of the planets are comparable and the eccentricities are small (e<0.1), the dynamics of the 2:1 and 3:2 planetary resonances is very similar. Finaly, the regions of transition between domains of the regimes of motion are characterized by chaotic motion.
Research support from Research Foundation of São Paulo State (FAPESP), Brazil (Proc. 98/13593-8).
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Bulletin of the American Astronomical Society, 34, #3< br> © 2002. The American Astronomical Soceity.