Irregular satellite capture during planetary resonance-crossing

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Passage of Jupiter and Saturn through the mutual 1:2 mean-motion resonance has recently been put forward as explanation of their relatively high eccentricities (Tsiganis et al. 2005, Nature 435, 459) and the orbital distribution of Jupiter's Trojans (Morbidelli et al. 2005, Nature 435, 462). Additional constraints on this kind of event recorded in other small-body populations would obviously be highly useful. Since some outer satellite orbits are known to be strongly affected by near-resonance of Jupiter and Saturn (``the Great Inequality"; Cuk and Burns 2004, AJ 128, 2518), the irregular satellites are natural candidates for such a study.
We have integrated 9200 test particles around both Jupiter and Saturn while they went through a 1:2 resonance-crossing event. The test particles were positioned on a grid in semimajor axes and inclinations, while their initial pericenters were placed at 0.01 AU from Saturn. The experiment's goal was to find out if short-lived bodies, spiraling into Saturn due to gas drag with an early circumplanetary disk could have had their pericenters raised by the resonant perturbations. We found that about 300 particles (3 percent) had their pericenters raised above 0.03 AU (the orbital distance of Iapetus) at Saturn, but the same happened for only 10 particles at Jupiter. The orbital distribution of the surviving particles at Saturn has strong similarities to that of the known irregular satellites.
We are currently exploring the applicability of this mechansm for Uranus, although its orbital history is more uncertain than Saturn's. We propose that lack of effect on Jovian satellites comes from the indirect nature of the perturbation, and will discuss the implications of these results for various resonance-crossing scenarios.

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