Hostname: page-component-586b7cd67f-g8jcs Total loading time: 0 Render date: 2024-11-24T10:40:50.148Z Has data issue: false hasContentIssue false
  • English
  • Français

Complex satellite systems: a general model of formation from rings

Published online by Cambridge University Press:  05 January 2015

Aurélien Crida  and
Sébastien Charnoz
Aurélien Crida
Affiliation:
Laboratoire Lagrange (UMR 7293), Université Nice Sophia-antipolis / CNRS / Observatoire de la Côte d'Azur, CS 34229, 06304 NICE cedex 4, FRANCE email: [email protected]
Sébastien Charnoz
Affiliation:
Laboratoire AIM (UMR 7158); Université Paris Diderot / CEA / IRFU-SAp, 91191 Gif-sur-Yvette cedex, FRANCE Institut Universitaire de France; 103 Bd Saint Michel, 75005 Paris, FRANCE
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Satellite systems are often seen as mini-planetary systems, and they are as various and complex. The Earth has one single satellite of more than one percent of its own mass, but the giant planets have many, some of them tiny. They constitute fascinating, interacting, evolving, and dynamically complex systems. While irregular satellites, having inclined and eccentric orbits, are supposed to be captured, it was generally admitted that regular satellites, having circular orbits in the equatorial plane of their host planet, formed in the gas and dust circum-planetary disk that surrounded giant planets at the time of their formation, more or less similarly as planets formed in the proto-planetary disk around their host star. Here, we propose an alternative mechanism for the formation of regular satellites: the spreading of a dynamically cold disk of solids beyond the Roche radius of a planet.

The Roche radius is defined as the distance from a planet beyond which self-gravity is stronger than tidal forces, allowing gravitationally bound aggregates to form, and satellites to exist. Saturn's rings are inside the Roche radius, which is why they don't coalesce into one single object. However, like any astrophysical disk in Keplerian rotation, they spread. Once material reaches the Roche limit, it should accrete into moonlets. These moonlets migrate outwards, repelled by tidal interactions with the rings and Saturn. We showed with numerical simulations that the small and mid-sized moons of Saturn formed this way, which explains their young age and composition (Charnoz et al.2010, 2011). Analytical calculations show that the formation of satellites from a ring of solids spreading beyond the Roche limit takes place in 2 phases: (i) the continuous regime, in which only one satellite forms (this regime prevailed for the moon-forming disk around the Earth); (ii) the pyramidal regime, in which a series of moons form, migrate outwards, merge. . . In this regime, the satellites should follow a precise mass-distance relation, which matches that of the Saturnian system, confirming that it formed this way. It also fits the Uranian and Neptunian systems, suggesting that these planets used to have massive rings that gave birth to their regular satellites, and vanished (Crida & Charnoz (2012)).

Refinements of this model, applications to planetary systems, and a recent likely observation of this process will be discussed in conclusion.

Keywords

planets and satellites: formationplanets and satellites: individual (Saturn)planets: rings
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S310: Complex Planetary Systems , July 2014 , pp. 182 - 189
Copyright
Copyright © International Astronomical Union 2014 

References

Canup, R. M. 2010, Nature, 468, 943.Google Scholar
Charnoz, S., Salmon, J., & Crida, A. 2010, Nature, 465, 752.Google Scholar
Charnoz, S., Crida, A., Castillo-Rogez, J., Lainey, V., Dones, L., Karatekin, Ö., Tobie, G., Mathis, S., Le Poncin-Lafitte, C., & Salmon, J. 2011, Icarus, 216, 535.Google Scholar
Crida, A. & Charnoz, S. 2010, Nature, 468, 903.Google Scholar
Crida, A. & Charnoz, S. 2012, Science, 338, 1196.Google Scholar
Crida, A. & Charnoz, S. 2013, SF2A-2013: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, 57.Google Scholar
Daisaka, H., Tanaka, H., & Ida, S. 2001, Icarus, 154, 296.Google Scholar
French, R. S. & Showalter, M. R. 2012, Icarus, 220, 911.Google Scholar
Lainey, V., Karatekin, Ö., Desmars, J., Charnoz, S., Arlot, J.-E., Emelyanov, N., Le Poncin-Lafitte, C., Mathis, S., Remus, F., Tobie, G., & Zahn, J.-P. 2012, ApJ, 752, 14.Google Scholar
Lin, D. N. C. & Papaloizou, J. 1979, MNRAS, 186, 799.Google Scholar
Lynden-Bell, D. & Pringle, J. E. 1974, MNRAS, 168, 603.Google Scholar
Murray, C. D., Cooper, N. J., Williams, G. A., Attree, N. O., & Boyer, J. S. 2014, Icarus, 236, 165.Google Scholar
Salmon, J., Charnoz, S., Crida, A. & Brahic, A. 2010 Icarus, 209, 771.Google Scholar