Some Effects of the Planetary Migration on the Satellites

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Recently, Tsiganis et al (2005) presented an interesting planetary migration theory. Among others results, according to the authors, a potential issue of their model, is the survivability of the inner satellites, while outer satellites could not survive the migration. In this work we investigate the stability of these satellites mainly in the case when Jupiter and Saturn were in 2:1 resonance. To save cpu time we adopt artificial migration models (linear and exponential) as well as static model (Michtchenko et al, 2001). In the case of the inner satellites, we concentrate on Uranus'retinue, more precisely, Oberon and others beyond it. The simulations confirm that in almost all cases, Oberon survives quite well (keeping its initial small eccentricity and inclination). For more distant satellites, in the static model, there are some examples where eccentricity are clearly excited and a few number of ejections. However when applying linear or exponential migration model, a lot of satellites beyond Oberon remain quite stable, with very small eccentricity, although the inclination may undergo some variation. In all these simulations, it is determinant the role played by the oblateness of the planet. Without considering it, the satellites are easily ejected. We also investigate some interesting cases of capture in resonance involving the precession of the node and the mean motion of the Sun. Finally, some numerical results of the dynamics of the outer satellites of Jupiter and Saturn during the migration, are presented.
Acknowledgements: The authors thank FAPESP, CNPQ, PIBIC and FUNDUNESP

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