Abstract
Planetary rings are the only nearby astrophysical disks and the only disks that have been investigated by spacecraft (especially the Cassini spacecraft orbiting Saturn). Although there are significant differences between rings and other disks, chiefly the large planet/ring mass ratio that greatly enhances the flatness of rings (aspect ratios as small as 10− 7), understanding of disks in general can be enhanced by understanding the dynamical processes observed at close range and in real time in planetary rings.We review the known ring systems of the four giant planets, as well as the prospects for ring systems yet to be discovered. We then review planetary rings by type. The A, B, and C rings of Saturn, plus the Cassini Division, comprise our solar system’s only dense broad disk and host many phenomena of general application to disks including spiral waves, gap formation, self-gravity wakes, viscous overstability and normal modes, impact clouds, and orbital evolution of embedded moons. Dense narrow rings are found both at Uranus (where they comprise the main rings entirely) and at Saturn (where they are embedded in the broad disk) and are the primary natural laboratory for understanding shepherding and self-stability. Narrow dusty rings, likely generated by embedded source bodies, are surprisingly found to sport azimuthally confined arcs at Neptune, Saturn, and Jupiter. Finally, every known ring system includes a substantial component of diffuse dusty rings.Planetary rings have shown themselves to be useful as detectors of planetary processes around them, including the planetary magnetic field and interplanetary impactors as well as the gravity of nearby perturbing moons. Experimental rings science has made great progress in recent decades, especially numerical simulations of self-gravity wakes and other processes but also laboratory investigations of coefficient of restitution and spectroscopic ground truth. The age of self-sustained ring systems is a matter of debate; formation scenarios are most plausible in the context of the early solar system, while signs of youthfulness indicate at least that rings have never been static phenomena.
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- 1.
The Laplace plane is the plane about which orbits precess. When the vertical motions of objects are damped by mutual collisions, material will settle into a ring centered on the Laplace plane.
- 2.
Throughout this work, we will use the word “dust” to refer to μm-sized particles regardless of their composition.
- 3.
The phase angle is formed by the Sun-object-observer lightpath. Dust-sized particles, having size comparable to the wavelength of visible light, tend to diffract light forward and are brightest at high phase angles. Larger objects tend to reflect light and are brightest at low phase angles.
- 4.
As recently formalized by the IAU, a “division” is defined as a region between two lettered rings that contains a sheet of material, while a “gap” is a clear region within a lettered ring that may or may not contain one or more ringlets (http://planetarynames.wr.usgs.gov/append8.html).
- 5.
Credit: G. H. Jones in JPL podcast, 6 March 2008 (http://www.jpl.nasa.gov/podcast/content.cfm?content=671)
- 6.
Here, we refer to the inclination of the planet’s equatorial plane with respect to the line of sight from Earth.
- 7.
along with the three planets of the HR 8799 system, announced at the same time
- 8.
For brevity, this discussion is limited to inner Lindblad resonances and inner vertical resonances, where the disk is inward of the forcing moon. Nearly all known spiral waves in rings are of this kind, though Tiscareno et al. (2007) detected inwardly propagating spiral density waves excited by outer Lindblad resonances with Pan.
- 9.
The azimuthal parameter m gives the number of spiral arms in the resonant wave pattern, while k + 1 is the “order” of the resonance, with first-order resonances generally being strongest, followed by second-order, etc.
- 10.
The exception is the nodal resonance, labeled − 1:0, in which the mean motion of the ring particles is resonant with the forcing moon’s nodal precession \({\dot{\Omega}}\). This peculiar resonance has a negative pattern speed, and its bending wave propagates outward (Rosen and Lissauer 1988).
- 11.
Moonlet wakes have little in common with self-gravity wakes (3.1.4), despite an unfortunate similarity in terminology.
- 12.
The periodicity of this alignment was recalculated by Chavez (2009), using updated orbital data.
- 13.
For Saturn’s Anthe and Methone arcs, as for Neptune’s Galatea arc, the circumferential ring is too faint to have been detected as yet but likely consists of material recently escaped from the arc-confining mechanism.
- 14.
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Acknowledgments
I thank Mark Showalter, Joe Burns, Josh Colwell, Jeff Cuzzi, Jonathan Fortney, Doug Hamilton, Matt Hedman, Doug Lin, Phil Nicholson, and John Weiss for helpful conversations. I additionally thank Robin Canup, John Cooper, Estelle Deau, Larry Esposito, and Rob French for valuable comments on the manuscript, and Hanno Rein for help in creating Fig. 7-3. I acknowledge funding from NASA Outer Planets Research (NNX10AP94G), NASA Cassini Data Analysis (NNX08AQ72G and NNX10AG67G), and the Cassini Project.
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Tiscareno, M.S. (2013). Planetary Rings. In: Oswalt, T.D., French, L.M., Kalas, P. (eds) Planets, Stars and Stellar Systems. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-5606-9_7
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