• DOI:10.1038/s41550-018-0616-8
• Corpus ID: 119236027

Ring dynamics around non-axisymmetric bodies with application to Chariklo and Haumea

@article{Sicardy2018RingDA,
  title={Ring dynamics around non-axisymmetric bodies with application to Chariklo and Haumea},
  author={Bruno Sicardy and Rodrigo Leiva and S. Renner and F. Roques and Maryame El Moutamid and Pablo Santos-Sanz and Josselin Desmars},
  journal={Nature Astronomy},
  year={2018},
  volume={3},
  pages={146-153}
}

• B. Sicardy, Rodrigo Leiva, +4 authors J. Desmars
• Published 19 November 2018
• Physics, Geology
• Nature Astronomy

Dense and narrow rings have been discovered recently around the small Centaur object Chariklo1 and the dwarf planet Haumea2, while being suspected around the Centaur Chiron3, although this point is debated4. They are the first rings observed in the Solar System elsewhere than around giant planets. In contrast to giant planets, gravitational fields of small bodies may exhibit large non-axisymmetric terms that create strong resonances between the spin of the object and the mean motion of ring particles. Here we show that modest topographic features or elongations of Chariklo and Haumea explain why their rings are relatively far away from the central body, when scaled to those of the giant planets5. Resonances actually clear on decadal timescales an initial collisional disk that straddles the corotation resonance (where the particles' mean motion matches the spin rate of the body). Quite generically, the disk material inside the corotation radius migrates onto the body, while the material outside the corotation radius is pushed outside the 1/2 resonance, where the particles complete one revolution while the body completes two rotations. Consequently, the existence of rings around non-axisymmetric bodies requires that the 1/2 resonance resides inside the Roche limit of the body, favouring faster rotators for being surrounded by rings.Chariklo, Haumea and potentially Chiron are the only known ringed Solar System objects that are not giant planets. The rings of these minor bodies are relatively further from their hosts than those around giant planets; this increase is shown to be due to resonances driven by modest topographic features or elongations.