News & Views | Published:

Solar System

Saturn's colossal ring

Nature volume 461, pages 10641065 (22 October 2009) | Download Citation

A hitherto undetected disk of debris around Saturn is the largest ever found to be orbiting a planet. This ring may hold the key to one of the most enigmatic landscapes in the Solar System.

On page 1098 of this issue, Verbiscer and colleagues1 report the discovery of an enormous ring around Saturn. The authors found this most tenuous of Saturn's known rings, which covers some 10,000 times as much area as the planet's photogenic main rings, by using the Spitzer Space Telescope to detect the ring's faint glow in the thermal infrared region of the electromagnetic spectrum. The ring is composed of dust, probably derived primarily from Saturn's distant moon Phoebe. Its discovery lends support to an earlier theory that dusty material from Phoebe is responsible for colouring the two-toned moon Iapetus.

This 'Phoebe ring' of Saturn (Fig. 1) is similar to previously known tenuous rings in the outer Solar System, such as Jupiter's gossamer rings or Saturn's E ring, in that it is composed mainly of small particles (less than 100 micrometres across) that must be constantly replenished from larger source bodies such as moons, because such tiny grains are eroded away or ejected from their host planet's orbit on very short timescales (less than 1,000 years). The Phoebe ring, like Jupiter's gossamer rings, probably consists of the dust ejected from moon surfaces by impacts2; by contrast, Saturn's E ring is supplied by geysers emanating from the interior of the planet's moon Enceladus.

Figure 1: Saturn's huge ring.
Figure 1

This diagram depicts the newly discovered1 'Phoebe ring' around Saturn, which spans at least 25 million kilometres and is the largest ring known to be orbiting a planet. The ring corresponds closely to the orbit of Phoebe, the largest of Saturn's outer 'irregular moons', and apparently the source of most of the ring's material. The ring is tilted owing to the influence of the Sun. Dust in the ring probably spirals inward and hits the leading hemisphere of the moon Iapetus, triggering that moon's distinctive two-toned coloration. Also shown are the orbit of Saturn's largest moon Titan, the planet itself and its other rings. Image: IMAGES COURTESY NASA/JPL-CALTECH

But the Phoebe ring is vastly different in scale from other dusty rings. It has a core radius (the distance from Saturn at which the ring's density reaches its peak value) that is about 200 times the radius of Saturn and 50 times that of the E ring, the previous record holder for the Solar System's largest planetary ring. Thanks to its huge dimensions, the Phoebe ring is at least ten times more massive than the E ring, despite having a particle number density (20 particles per cubic kilometre) that is tens of millions of times lower1.

The destiny of all that mass may be the most interesting aspect of the Phoebe ring's discovery. Just as the icy dust in the E ring spreads out from Enceladus and seems to brightly coat the surfaces of Saturn's inner moons3, so the dust in the Phoebe ring is expected to spiral inward towards Saturn, where much of it would be swept up by Iapetus, the outermost of Saturn's large moons, whose surface patterns are a 300-year-old mystery.

Because Iapetus keeps one face always towards its parent planet, like most moons in the Solar System, it also keeps one face (the 'leading hemisphere') directed towards its direction of motion. Iapetus' leading hemisphere is among the darkest surfaces in the Solar System (its albedo — the fraction of sunlight that is reflected back into space — is about 4%), whereas the opposite ('trailing') hemisphere and the poles are quite bright. Surfaces of intermediate brightness, however, are almost entirely absent4. It has long been considered plausible that dust from Phoebe is the most likely cause of Iapetus' curious coloration5,6, but broad agreement has been elusive. The spectral match between the two is not exact, and it is unclear whether the differences can be explained by dust deposition at hyper-velocity and subsequent mixing with the native Iapetan surface.

Furthermore, the lack of dark material at Iapetus' poles is unexpected under a simple model of infalling pollution, although this might be explained by a model that includes infall plus subsequent thermal processing. On the other hand, the leading alternative theory — that the dark material somehow comes from within Iapetus — has a difficult time explaining the close alignment of the dark terrain with the leading hemisphere. Verbiscer and colleagues' discovery1 of a disk of material surrounding Saturn, corresponding to Phoebe's orbit, is strong evidence for an external source for the dark material on Iapetus. However, much work remains to be done to determine the origin and fate of the observed dust.

As it spirals inward, some fraction of the Phoebe ring's dust makes it past Iapetus and continues on towards the next likely targets, the moons Hyperion and Titan. But the chaotic rotation of Hyperion7 would cause it to become evenly coated with the ring's dust, not asymmetrically as for Iapetus, and for Titan the infall would be just one more component of its already complex surface chemistry8.

Further observations of this enormous ring would be highly desirable to better determine its structure and spectral properties. In particular, complementary photometry (measurement of an object's brightness) in visible light would constrain the size distribution and albedos of its component particles — are they really as dark as their presumed source (Phoebe) and destination (Iapetus' leading hemisphere)? Furthermore, such observations could clarify whether other moons besides Phoebe are supplying this ring with dust. Phoebe is by far the largest of Saturn's distant moons, but this does not necessarily make it the best source of dust. Although bigger moons present larger targets for dust-generating impacts, their increased surface gravity correspondingly holds on to a greater fraction of ejecta, so the best-sized moon for making dust is not obvious2.

The data presented by Verbiscer et al.1 provide good evidence that this newly discovered ring does in fact ultimately originate from Phoebe in particular: the ring's vertical profile (seen nearly edge-on from Earth) exhibits a double-layered structure whose thickness corresponds to the vertical distance spanned by Phoebe as it goes along its inclined orbit. This structure is very similar to that of Jupiter's rings and just the sort of profile expected for a population of dust particles originating from Phoebe2. It may be, as Verbiscer et al.1 argue, that Phoebe's contribution has been enhanced by primordial large collisions9,10 that generated centimetre-sized and larger chunks of ice and rock that can remain in place over the age of the Solar System. These chunks in turn would generate dust that is ultimately derived from Phoebe and that preserves its orbital characteristics. However, it may well be that Phoebe's little brothers and sisters among Saturn's distant moons also play a significant part in generating the dust that makes up the observed ring, and thus in determining the chemistry of Iapetus.

Whereas nearly everything in the Solar System rotates and orbits in an anticlockwise direction as seen from above, the Phoebe ring almost certainly rotates backwards ('retrograde'), the first ring known to do so. It is also the first ring known to be significantly tilted (by 27°) to its parent planet's equator. Both of these characteristics are due to the ring's source bodies, Saturn's distant moons, many of which (including Phoebe) have retrograde orbits that are more affected by the Sun than by Saturn's equatorial bulge.

The possibility of giant rings existing around other planets is also worth exploring. Jupiter's moon Himalia is only slightly smaller than Phoebe, and whereas Callisto's coloration is less extreme than Iapetus' in both contrast and distribution, Callisto does have bright and dark terrains, and shows spectral differences between its leading and trailing hemispheres11. Future observations may therefore reveal giant rings at Jupiter and elsewhere, or may show that Saturn's giant ring is as unique as its more famous main rings.


  1. 1.

    , & Nature 461, 1098–1100 (2009).

  2. 2.

    et al. Science 284, 1146–1150 (1999).

  3. 3.

    et al. Science 315, 815 (2007).

  4. 4.

    et al. Science 307, 1237–1242 (2005).

  5. 5.

    IAU Colloq. 28, abstr. (1974).

  6. 6.

    , , & Astron. Soc. Pacif. Conf. Ser. 104B, 179–182 (1996).

  7. 7.

    , & Icarus 58, 137–152 (1984).

  8. 8.

    & Annu. Rev. Earth Planet. Sci. 37, 299–320 (2009).

  9. 9.

    , , & Astron. J. 126, 398–429 (2003).

  10. 10.

    , & Mon. Not. R. Astron. Soc. 392, 455–474 (2009).

  11. 11.

    et al. in Jupiter: The Planet, Satellites, and Magnetosphere (eds Bagenal, F., Dowling, T. E. & McKinnon, W. B.) 397–426 (Cambridge Univ. Press, 2003).

Download references

Author information


  1. Matthew S. Tiscareno and Matthew M. Hedman are in the Department of Astronomy, Cornell University, Ithaca, New York 14853, USA.

    • Matthew S. Tiscareno
    •  & Matthew M. Hedman


  1. Search for Matthew S. Tiscareno in:

  2. Search for Matthew M. Hedman in:

About this article

Publication history




By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.

Newsletter Get the most important science stories of the day, free in your inbox. Sign up for Nature Briefing