[Previous] | [Session 30] | [Next]
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 S�o Paulo State (FAPESP), Brazil (Proc. 98/13593-8).
If the author provided an email address or URL for general inquiries,
it is as follows:
Bulletin of the American Astronomical Society, 34, #3< br> © 2002. The American Astronomical Soceity.