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Moons of Saturn

Artist's concepts of the Saturnian ring–moon system
Saturn, its rings and major icy moons—from Mimas to Rhea
Images of several moons of Saturn. From left to right: Mimas, Enceladus, Tethys, Dione, Rhea; Titan in the background; Iapetus (top) and irregularly shaped Hyperion (bottom). Some small moons are also shown. All to scale.

The moons of Saturn are numerous and diverse ranging from tiny moonlets less than 1 kilometer across to the enormous Titan, which is larger than the planet Mercury. Saturn has 62 moons with confirmed orbits, 53 of which have names and only 13 of which have diameters larger than 50 kilometers.[1][2][3] Seven Saturnian moons are large enough to be ellipsoidal in shape, though only two of those, Titan and Rhea, are currently in hydrostatic equilibrium, as well as dense rings with complex orbital motions of their own. Particularly notable among Saturn's moons are Titan, the second-largest moon (after Jupiter's Ganymede) in the Solar System, with a nitrogen-rich Earth-like atmosphere and a landscape including hydrocarbon lakes and dry river networks;[4] and Enceladus, which is seemingly similar in chemical makeup to comets,[5] emits jets of gas and dust and may harbor liquid water under its south pole region.[6]

Twenty-four of Saturn's moons are regular satellites; they have prograde orbits not greatly inclined to Saturn's equatorial plane.[7] They include the seven major satellites, four small moons that exist in a trojan orbit with larger moons, two mutually co-orbital moons and two moons that act as shepherds of Saturn's F Ring. Two other known regular satellites orbit within gaps in Saturn's rings. The relatively large Hyperion is locked in a resonance with Titan. The remaining regular moons orbit near the outer edge of the A Ring, within G Ring and between the major moons Mimas and Enceladus. The regular satellites are traditionally named after Titans and Titanesses or other figures associated with the mythological Saturn.

The remaining 38, all small except one, are irregular satellites, whose orbits are much farther from Saturn, have high inclinations, and are mixed between prograde and retrograde. These moons are probably captured minor planets, or debris from the breakup of such bodies after they were captured, creating collisional families. The irregular satellites have been classified by their orbital characteristics into the Inuit, Norse, and Gallic groups, and their names are chosen from the corresponding mythologies. The largest of the irregular moons is Phoebe, the ninth moon of Saturn, discovered at the end of the 19th century.

The rings of Saturn are made up of objects ranging in size from microscopic to moonlets hundreds of meters across, each in its own orbit around Saturn.[8] Thus a precise number of Saturnian moons cannot be given, because there is no objective boundary between the countless small anonymous objects that form Saturn's ring system and the larger objects that have been named as moons. Over 150 moonlets embedded in the rings have been detected by the disturbance they create in the surrounding ring material, though this is thought to be only a small sample of the total population of such objects.[9]

Discovery and naming

Saturn (overexposed) and the moons Iapetus, Titan, Dione, Hyperion, and Rhea viewed through a 12.5-inch telescope

Early observations

Before the advent of telescopic photography, eight moons of Saturn were discovered by direct observation using optical telescopes. Saturn's largest moon, Titan, was discovered in 1655 by Christiaan Huygens using a Script error: No such module "convert". objective lens[10] on a refracting telescope of his own design.[11] Tethys, Dione, Rhea and Iapetus (the "Sidera Lodoicea") were discovered between 1671 and 1684 by Giovanni Domenico Cassini.[12] Mimas and Enceladus were discovered in 1789 by William Herschel.[12] Hyperion was discovered in 1848 by W.C. Bond, G.P. Bond[13] and William Lassell.[14]

The use of long-exposure photographic plates made possible the discovery of additional moons. The first to be discovered in this manner, Phoebe, was found in 1899 by W.H. Pickering.[15] In 1966 the tenth satellite of Saturn was discovered by Audouin Dollfus, when the rings were observed edge-on near an equinox.[16] It was later named Janus. A few years later it was realized that all observations of 1966 could only be explained if another satellite had been present and that it had an orbit similar to that of Janus.[16] This object is now known as Epimetheus, the eleventh moon of Saturn. It shares the same orbit with Janus—the only known example of co-orbitals in the Solar System.[17] In 1980 three additional Saturnian moons were discovered from the ground and later confirmed by the Voyager probes. They are trojan moons of Dione (Helene) and Tethys (Telesto and Calypso).[17]

Observations by spacecraft

Four moons of Saturn can be seen on this image by the Cassini spacecraft: Huge Titan and Dione at the bottom, small Prometheus (under the rings) and tiny Telesto above center.
Five moons in another Cassini image: Rhea bisected in the foreground, Mimas behind it, bright Enceladus above and beyond the rings, Pandora eclipsed by the F Ring, and Janus off to the left.

The study of the outer planets has since been revolutionized by the use of unmanned space probes. The arrival of the Voyager spacecraft at Saturn in 1980–1981 resulted in the discovery of three additional moons—Atlas, Prometheus and Pandora, bringing the total to 17.[17] In addition, Epimetheus was confirmed as distinct from Janus. In 1990, Pan was discovered in archival Voyager images.[17]

The Cassini mission, which arrived at Saturn in the summer of 2004, initially discovered three small inner moons including Methone and Pallene between Mimas and Enceladus as well as the second Lagrangian moon of Dione—Polydeuces. It also observed three suspected but unconfirmed moons in the F Ring.[18] In November 2004 Cassini scientists announced that the structure of Saturn's rings indicates the presence of several more moons orbiting within the rings, although only one, Daphnis, has been visually confirmed so far (in 2005).[19] In 2007 Anthe was announced.[20] In 2008 it was reported that Cassini observations of a depletion of energetic electrons in Saturn's magnetosphere near Rhea might be the signature of a tenuous ring system around Saturn's second largest moon.[21] In March 2009, Aegaeon, a moonlet within the G Ring, was announced.[22] In July of the same year, S/2009 S 1, the first moonlet within the B Ring, was observed.[3] In April 2014, the possible beginning of a new moon, within the A Ring, was reported.[23] (related image)

Outer moons

File:Quadruple Saturn moon transit.jpg
Quadruple Saturn–moon transit captured by the Hubble Space Telescope

Study of Saturn's moons has also been aided by advances in telescope instrumentation, primarily the introduction of digital charge-coupled devices which replaced photographic plates. For the entire 20th century, Phoebe stood alone among Saturn's known moons with its highly irregular orbit. Beginning in 2000, however, three dozen additional irregular moons have been discovered using ground-based telescopes.[24] A survey starting in late 2000 and conducted using three medium-size telescopes found thirteen new moons orbiting Saturn at a great distance, in eccentric orbits, which are highly inclined to both the equator of Saturn and the ecliptic.[25] They are probably fragments of larger bodies captured by Saturn's gravitational pull.[24][25] In 2005, astronomers using the Mauna Kea Observatory announced the discovery of twelve more small outer moons.[26][27] In 2006, astronomers using the Subaru 8.2 m telescope reported the discovery of further nine irregular moons.[28] In April 2007, Tarqeq (S/2007 S 1) was announced. In May of the same year S/2007 S 2 and S/2007 S 3 were reported.[29]


Main article: Naming of moons

The modern names for Saturnian moons were suggested by John Herschel in 1847.[12] He proposed to name them after mythological figures associated with the Roman god of agriculture and harvest, Saturn (equated to the Greek Cronus).[12] In particular, the then known seven satellites were named after Titans, Titanesses and Giants—brothers and sisters of Cronus.[15] In 1848 Lassell proposed that the eighth satellite of Saturn was named Hyperion after another Titan.[14] When in the 20th century the names of Titans were exhausted, the moons were named after different characters of the Greco-Roman mythology or giants from other mythologies.[30] All the irregular moons (except Phoebe) are named after Inuit and Gallic gods and after Norse ice giants.[31]

Some asteroids share the same names as moons of Saturn: 55 Pandora, 106 Dione, 577 Rhea, 1809 Prometheus, 1810 Epimetheus, and 4450 Pan. In addition, two more asteroids previously shared the names of Saturnian moons until spelling differences were made permanent by the International Astronomical Union (IAU): Calypso and asteroid 53 Kalypso; and Helene and asteroid 101 Helena.


File:Masses of Saturnian moons.png
The relative masses of Saturn's moons. Mimas, the rings, and the small moons are invisible at this scale.

Saturn's satellite system is very lopsided: one moon, Titan, comprises more than 96% of the mass in orbit around the planet. The six other planemo (ellipsoidal) moons constitute roughly 4% of the mass, and the remaining 55 small moons, together with the rings, comprise only 0.04%.[a]

Saturn's major satellites, compared to the Moon
Orbital radius
Orbital period
Mimas 396
(12% Moon)
(0.05% Moon)
(48% Moon)
(3% Moon)
Enceladus 504
(14% Moon)
(0.2% Moon)
(62% Moon)
(5% Moon)
Tethys 1,062
(30% Moon)
(0.8% Moon)
(77% Moon)
(7% Moon)
Dione 1,123
(32% Moon)
(1.5% Moon)
(98% Moon)
(10% Moon)
Rhea 1,527
(44% Moon)
(3% Moon)
(137% Moon)
(20% Moon)
Titan 5,150
(148% Moon)
(75% Mars)
(180% Moon)
(318% Moon)
(60% Moon)
Iapetus 1,470
(42% Moon)
(2.5% Moon)
(926% Moon)
(290% Moon)

Orbital groups

Although the boundaries may be somewhat vague, Saturn's moons can be divided into ten groups according to their orbital characteristics. Many of them, such as Pan and Daphnis, orbit within Saturn's ring system and have orbital periods only slightly longer than the planet's rotation period.[35] The innermost moons and most regular satellites all have mean orbital inclinations ranging from less than a degree to about 1.5 degrees (except Iapetus, which has an inclination of 7.57 degrees) and small orbital eccentricities.[36] On the other hand, irregular satellites in the outermost regions of Saturn's moon system, in particular the Norse group, have orbital radii of millions of kilometers and orbital periods lasting several years. The moons of the Norse group also orbit in the opposite direction to Saturn's rotation.[31]

Ring moonlets

Main article: Rings of Saturn
File:PIA08319 Daphnis in Keeler Gap.jpg
Daphnis in the Keeler gap

During late July 2009, a moonlet was discovered in the B Ring,[3] 480 km from the outer edge of the ring, by the shadow it cast. It is estimated to be 300 m in diameter. Unlike the A Ring moonlets (see below), it does not induce a 'propeller' feature, probably due to the density of the B Ring.[37]

Possible beginning of a new moon of Saturn imaged on 15 April 2014

In 2006, four tiny moonlets were found in Cassini images of the A Ring.[38] Before this discovery only two larger moons had been known within gaps in the A Ring: Pan and Daphnis. These are large enough to clear continuous gaps in the ring.[38] In contrast, a moonlet is only massive enough to clear two small—about 10 km across—partial gaps in the immediate vicinity of the moonlet itself creating a structure shaped like an airplane propeller.[39] The moonlets themselves are tiny, ranging from about 40 to 500 meters in diameter, and are too small to be seen directly.[9] In 2007, the discovery of 150 more moonlets revealed that they (with the exception of two that have been seen outside the Encke gap) are confined to three narrow bands in the A Ring between 126,750 and 132,000 km from Saturn's center. Each band is about a thousand kilometers wide, which is less than 1% the width of Saturn's rings.[9] This region is relatively free from the disturbances caused by resonances with larger satellites,[9] although other areas of the A Ring without disturbances are apparently free of moonlets. The moonlets were probably formed from the breakup of a larger satellite.[39] It is estimated that the A Ring contains 7,000–8,000 propellers larger than 0.8 km in size and millions larger than 0.25 km.[9]

Similar moonlets may reside in the F Ring.[9] There, "jets" of material may be due to collisions, initiated by perturbations from the nearby small moon Prometheus, of these moonlets with the core of the F Ring. One of the largest F-Ring moonlets may be the as-yet unconfirmed object S/2004 S 6. The F Ring also contains transient "fans" which are thought to result from even smaller moonlets, about 1 km in diameter, orbiting near the F Ring core.[40]

One of the recently discovered moons, Aegaeon, resides within the bright arc of G Ring and is trapped in the 7:6 mean-motion resonance with Mimas.[22] This means that it makes exactly seven revolutions around Saturn while Mimas makes exactly six. The moon is the largest among the population of bodies that are sources of dust in this ring.[41]

In April 2014, NASA scientists reported the possible beginning of a new moon, within the A Ring, of the planet Saturn.[23] (related image)

Ring shepherds

Main article: Rings of Saturn

Shepherd satellites are small moons that orbit within, or just beyond, a planet's ring system. They have the effect of sculpting the rings: giving them sharp edges, and creating gaps between them. Saturn's shepherd moons are Pan (Encke gap), Daphnis (Keeler gap), Atlas (A Ring), Prometheus (F Ring) and Pandora (F Ring).[18][22] These moons together with co-orbitals (see below) probably formed as a result of accretion of the friable ring material on preexisting denser cores. The cores with sizes from one-third to one-half the present day moons may be themselves collisional shards formed when a parental satellite of the rings disintegrated.[35]


Main article: Co-orbital moon

Janus and Epimetheus are called co-orbital moons.[17] They are of roughly equal size, with Janus being slightly larger than Epimetheus.[35] Janus and Epimetheus have orbits with only a few kilometers difference in semi-major axis, close enough that they would collide if they attempted to pass each other. Instead of colliding, however, their gravitational interaction causes them to swap orbits every four years.[42]

Inner large moons

The innermost large moons of Saturn orbit within its tenuous E Ring, along with three smaller moons of the Alkyonides group.

  • Mimas is the smallest and least massive of the inner round moons,[33] although its mass is sufficient to alter the orbit of Methone.[42] It is noticeably ovoid-shaped, having been made shorter at the poles and longer at the equator (by about 20 km) by the effects of Saturn's gravity.[43] Mimas has a large impact crater one-third its diameter, Herschel, situated on its leading hemisphere.[44] Mimas has no known past or present geologic activity, and its surface is dominated by impact craters. The only tectonic features known are a few arcuate and linear troughs, which probably formed when Mimas was shattered by the Herschel impact.[44]
File:Enceladus south pole SE15.png
Tiger stripes on Enceladus
  • Enceladus is one of the smallest of Saturn's moons that is spherical in shape—only Mimas is smaller[43]—yet is the only small Saturnian moon that is currently endogenously active, and the smallest known body in the Solar System that is geologically active today.[45] Its surface is morphologically diverse; it includes ancient heavily cratered terrain as well as younger smooth areas with few impact craters. Many plains on Enceladus are fractured and intersected by systems of lineaments.[45] The area around its south pole was found by Cassini to be unusually warm and cut by a system of fractures about 130 km long called "tiger stripes", some of which emit jets of water vapor and dust.[45] These jets form a large plume off its south pole, which replenishes Saturn's E ring[45] and serves as the main source of ions in the magnetosphere of Saturn.[46] The gas and dust are released with a rate of more than 100 kg/s. Enceladus may have liquid water underneath the south-polar surface.[45] The source of the energy for this cryovolcanism is thought to be a 2:1 mean-motion resonance with Dione.[45] The pure ice on the surface makes Enceladus one of the brightest known objects in the Solar System—its geometrical albedo is more than 140%.[45]
  • Tethys is the third largest of Saturn's inner moons.[33] Its most prominent features are a large (400 km diameter) impact crater named Odysseus on its leading hemisphere and a vast canyon system named Ithaca Chasma extending at least 270° around Tethys.[44] The Ithaca Chasma is concentric with Odysseus, and these two features may be related. Tethys appears to have no current geological activity. A heavily cratered hilly terrain occupies the majority of its surface, while a smaller and smoother plains region lies on the hemisphere opposite to that of Odysseus.[44] The plains contain fewer craters and are apparently younger. A sharp boundary separates them from the cratered terrain. There is also a system of extensional troughs radiating away from Odysseus.[44] The density of Tethys (0.985 g/cm3) is less than that of water, indicating that it is made mainly of water ice with only a small fraction of rock.[32]
  • Dione is the second-largest inner moon of Saturn. It has a higher density than the geologically dead Rhea, the largest inner moon, but lower than that of active Enceladus.[43] While the majority of Dione's surface is heavily cratered old terrain, this moon is also covered with an extensive network of troughs and lineaments, indicating that in the past it had global tectonic activity.[47] The troughs and lineaments are especially prominent on the trailing hemisphere, where several intersecting sets of fractures form what is called "wispy terrain".[47] The cratered plains have a few large impact craters reaching 250 km in diameter.[44] Smooth plains with low impact-crater counts are present as well on a small fraction its surface.[48] They were probably tectonically resurfaced relatively later in the geological history of Dione. At two locations within smooth plains strange landforms (depressions) resembling oblong impact craters have been identified, both of which lie at the centers of radiating networks of cracks and troughs;[48] these features may be cryovolcanic in origin. Dione may be geologically active even now, although on a scale much smaller than the cryovolcanism of Enceladus. This follows from Cassini magnetic measurements that show Dione is a net source of plasma in the magnetosphere of Saturn, much like Enceladus.[48]


File:Methone PIA14633.jpg
Cassini image of Methone's leading side taken on 20 May 2012

Three small moons orbit between Mimas and Enceladus: Methone, Anthe, and Pallene. Named after the Alkyonides of Greek mythology, they are some of the smallest moons in the Saturn system. Anthe and Methone possess very faint ring arcs along their orbits while Pallene possesses a faint complete ring.[49] Of these three moons, only Methone has been photographed at close range, showing it to be egg-shaped with very few or no craters.[50]

Trojan moons

Main article: Trojan moon

Trojan moons are a unique feature only known from the Saturnian system. A trojan body orbits at either the leading L4 or trailing L5 Lagrange point of a much larger object, such as a large moon or planet. Tethys has two trojan moons, Telesto (leading) and Calypso (trailing), and Dione also has two, Helene (leading) and Polydeuces (trailing).[18] Helene is by far the largest trojan moon,[43] while Polydeuces is the smallest and has the most chaotic orbit.[42] These moons are coated with dusty material that has smoothened out their surfaces.[51]

Outer large moons

These moons all orbit beyond the E Ring. They are:

File:PIA08148 (Rhea-Splat).jpg
Inktomi or "The Splat", a relatively young crater with prominent butterfly-shaped ejecta on Rhea's leading hemisphere
  • Rhea is the second-largest of Saturn's moons.[43] In 2005 Cassini detected a depletion of electrons in the plasma wake of Rhea, which forms when the co-rotating plasma of Saturn's magnetosphere is absorbed by the moon.[21] The depletion was hypothesized to be caused by the presence of dust-sized particles concentrated in a few faint equatorial rings.[21] Such a ring system would make Rhea the only moon in the Solar System known to have rings.[21] However, subsequent targeted observations of the putative ring plane from several angles by Cassini's narrow-angle camera turned up no evidence of the expected ring material, leaving the origin of the plasma observations unresolved.[52] Otherwise Rhea has rather a typical heavily cratered surface,[44] with the exceptions of a few large Dione-type fractures (wispy terrain) on the trailing hemisphere[53] and a very faint "line" of material at the equator that may have been deposited by material deorbiting from present or former rings.[54] Rhea also has two very large impact basins on its anti-Saturnian hemisphere, which are about 400 and 500 km across.[53] The first, Tirawa, is roughly comparable to the Odysseus basin on Tethys.[44] There is also a 48 km-diameter impact crater called Inktomi[55][b] at 112°W that is prominent because of an extended system of bright rays,[56] which may be one of the youngest craters on the inner moons of Saturn.[53] No evidence of any endogenic activity has been discovered on the surface of Rhea.[53]
  • Titan, at 5,150 km diameter, is the second largest moon in the Solar System and Saturn's largest.[33] Out of all the large moons, Titan is the only one with a dense (surface pressure of 1.5 atm), cold atmosphere, primarily made of nitrogen with a small fraction of methane.[57] The dense atmosphere frequently produces bright white convective clouds, especially over the south pole region.[57] On June 6, 2013, scientists at the IAA-CSIC reported the detection of polycyclic aromatic hydrocarbons in the upper atmosphere of Titan.[58] On June 23, 2014, NASA claimed to have strong evidence that nitrogen in the atmosphere of Titan came from materials in the Oort cloud, associated with comets, and not from the materials that formed Saturn in earlier times.[59] The surface of Titan, which is difficult to observe due to persistent atmospheric haze, shows only a few impact craters and is probably very young.[57] It contains a pattern of light and dark regions, flow channels and possibly cryovolcanos.[57][60] Some dark regions are covered by longitudinal dune fields shaped by tidal winds, where sand is made of frozen water or hydrocarbons.[61] Titan is the only body in the Solar System beside Earth with bodies of liquid on its surface, in the form of methane–ethane lakes in Titan's north and south polar regions.[62] The largest lake, Kraken Mare, is larger than the Caspian Sea.[63] Like Europa and Ganymede, it is believed that Titan has a subsurface ocean made of water mixed with ammonia, which can erupt to the surface of the moon and lead to cryovolcanism.[60] On July 2, 2014, NASA reported the ocean inside Titan may be "as salty as the Earth's Dead Sea".[64][65]
  • Hyperion is Titan's nearest neighbor in the Saturn system. The two moons are locked in a 4:3 mean-motion resonance with each other, meaning that while Titan makes four revolutions around Saturn, Hyperion makes exactly three.[33] With an average diameter of about 270 km, Hyperion is smaller and lighter than Mimas.[66] It has an extremely irregular shape, and a very odd, tan-colored icy surface resembling a sponge, though its interior may be partially porous as well.[66] The average density of about 0.55 g/cm3[66] indicates that the porosity exceeds 40% even assuming it has a purely icy composition. The surface of Hyperion is covered with numerous impact craters—those with diameters 2–10 km are especially abundant.[66] It is the only moon known to have a chaotic rotation, which means Hyperion has no well-defined poles or equator. While on short timescales the satellite approximately rotates around its long axis at a rate of 72–75° per day, on longer timescales its axis of rotation (spin vector) wanders chaotically across the sky.[66] This makes the rotational behavior of Hyperion essentially unpredictable.[67]
File:Iapetus equatorial ridge.jpg
Equatorial ridge on Iapetus
  • Iapetus is the third-largest of Saturn's moons.[43] Orbiting the planet at 3.5 million km, it is by far the most distant of Saturn's large moons, and also possesses the greatest orbital inclination, at 15.47°.[34] Iapetus has long been known for its unusual two-toned surface; its leading hemisphere is pitch-black and its trailing hemisphere is almost as bright as fresh snow.[68] Cassini images showed that the dark material is confined to a large near equatorial area on the leading hemisphere called Cassini Regio, which extends approximately from 40°N to 40°S.[68] The pole regions of Iapetus are as bright as its trailing hemisphere. Cassini also discovered a 20 km tall equatorial ridge, which spans nearly the moon's entire equator.[68] Otherwise both dark and bright surfaces of Iapetus are old and heavily cratered. The images revealed at least four large impact basins with diameters from 380 to 550 km and numerous smaller impact craters.[68] No evidence of any endogenic activity has been discovered.[68] A clue to the origin of the dark material covering part of Iapetus's starkly dichromatic surface may have been found in 2009, when NASA's Spitzer Space Telescope discovered a vast, nearly invisible disk around Saturn, just inside the orbit of the moon Phoebe—the Phoebe ring.[69] Scientists believe that the disk originates from dust and ice particles kicked up by impacts on Phoebe. Because the disk particles, like Phoebe itself, orbit in the opposite direction to Iapetus, Iapetus collides with them as they drift in the direction of Saturn, darkening its leading hemisphere slightly.[69] Once a difference in albedo, and hence in average temperature, was established between different regions of Iapetus, a thermal runaway process of water ice sublimation from warmer regions and deposition of water vapor onto colder regions ensued. Iapetus's present two-toned appearance results from the contrast between the bright, primarily ice-coated areas and regions of dark lag, the residue left behind after the loss of surface ice.[70][71]

Irregular moons

File:Saturn's irregular satellites.png
Diagram illustrating the orbits of the irregular satellites of Saturn. The inclination and semi-major axis are represented on the Y and X-axis, respectively. The eccentricity of the orbits is shown by the segments extending from the pericenter to apocenter. The satellites with positive inclinations are prograde, those with negative are retrograde. The X-axis is labeled in km. The prograde Inuit and Gallic groups and the retrograde Norse group are identified.

Irregular moons are small satellites with large-radii, inclined, and frequently retrograde orbits, believed to have been acquired by the parent planet through a capture process. They often occur as collisional families or groups.[24] The precise size as well as albedo of the irregular moons are not known for sure because the moons are very small to be resolved by a telescope, although the latter is usually assumed to be quite low—around 6% (albedo of Phoebe) or less.[25] The irregulars generally have featureless visible and near infrared spectra dominated by water absorption bands.[24] They are neutral or moderately red in color—similar to C-type, P-type, or D-type asteroids,[31] though they are much less red than Kuiper belt objects.[24][c]

Inuit group

The Inuit group includes five prograde outer moons that are similar enough in their distances from the planet (186–297 radii of Saturn), their orbital inclinations (45–50°) and their colors that they can be considered a group.[25][31] The moons are Ijiraq, Kiviuq, Paaliaq, Siarnaq, and Tarqeq.[31] The largest among them is Siarnaq with an estimated size of about 40 km.

Gallic group

The Gallic group are four prograde outer moons that are similar enough in their distance from the planet (207–302 radii of Saturn), their orbital inclination (35–40°) and their color that they can be considered a group.[25][31] They are Albiorix, Bebhionn, Erriapus, and Tarvos.[31] Tarvos, as of 2009, is the most distant of Saturn's moons with a prograde orbit. The largest among these moons is Albiorix with an estimated size of about 32 km.

Norse group

The Norse (or Phoebe) group consists of 29 retrograde outer moons.[25][31] They are Aegir, Bergelmir, Bestla, Farbauti, Fenrir, Fornjot, Greip, Hati, Hyrrokkin, Jarnsaxa, Kari, Loge, Mundilfari, Narvi, Phoebe, Skathi, Skoll, Surtur, Suttungr, Thrymr, Ymir, S/2004 S 7, S/2004 S 12, S/2004 S 13, S/2004 S 17, S/2006 S 1, S/2006 S 3, S/2007 S 2, and S/2007 S 3.[31] After Phoebe, Ymir is the largest of the known retrograde irregular moons, with an estimated diameter of only 18 km. The Norse group may itself consist of several smaller subgroups.[31]

  • Phoebe, at 214 km in diameter, is by far the largest of Saturn's irregular satellites.[24] It has a retrograde orbit and rotates on its axis every 9.3 hours.[72] Phoebe was the first moon of Saturn to be studied in detail by Cassini, in June 2004; during this encounter Cassini was able to map nearly 90% of the moon's surface. Phoebe has a nearly spherical shape and a relatively high density of about 1.6 g/cm3.[24] Cassini images revealed a dark surface scarred by numerous impacts—there are about 130 craters with diameters exceeding 10 km. Spectroscopic measurement showed that the surface is made of water ice, carbon dioxide, phyllosilicates, organics and possibly iron bearing minerals.[24] Phoebe is believed to be a captured centaur that originated in the Kuiper belt.[24] It also serves as a source of material for the largest known ring of Saturn, which darkens the leading hemisphere of Iapetus (see above).[69]


Confirmed moons

The Saturnian moons are listed here by orbital period (or semi-major axis), from shortest to longest. Moons massive enough for their surfaces to have collapsed into a spheroid are highlighted in bold, while the irregular moons are listed in red, orange and gray background.

Major icy moons


Inuit group

Gallic group

Norse group

Order Label
Name Pronunciation (key) Image Diameter (km)[e] Mass
(×1015 kg) [f]
Semi-major axis (km) [g] Orbital period (d)[g][h] Inclination [g][i] Eccentricity Position Discovery
1 S/2009 S/2009 S 1 50px ≈ 0.3 < 0.0001 ≈ 117000 ≈ 0.47 ≈ 0° ≈ 0 outer B Ring 2009 Cassini–Huygens[3]
(moonlets) 50px 0.04 to 0.4 (Earhart) < 0.0001 ≈ 130000 ≈ 0.55 ≈ 0° ≈ 0 Three 1000 km bands within A Ring 2006 Cassini–Huygens
2 XVIII Pan Pan ˈpæn 50px 28.2±2.6
(34 × 31 × 20)
4.95±0.75 133584 +0.57505 0.001° 0.000035 in Encke Division 1990 M. Showalter
3 XXXV Daphnis Daphnis ˈdæfnɨs 50px 7.6±1.6
(9 × 8 × 6)
0.084±0.012 136505 +0.59408 ≈ 0° ≈ 0 in Keeler Gap 2005 Cassini–Huygens
4 XV Atlas Atlas ˈætləs 50px 30.2±1.8
(41 × 35 × 19)
6.6±0.045 137670 +0.60169 0.003° 0.0012 outer A Ring shepherd 1980 Voyager 2
5 XVI Prometheus Prometheus proʊˈmiːθiːəs 50px 86.2±5.4
(136 × 79 × 59)
159.5±1.5 139380 +0.61299 0.008° 0.0022 inner F Ring shepherd 1980 Voyager 2
6 XVII Pandora Pandora pænˈdɔərə 30px 81.4±3.0
(104 × 81 × 64)
137.1±1.9 141720 +0.62850 0.050° 0.0042 outer F Ring Shepherd 1980 Voyager 2
7a XI Epimetheus Epimetheus ˌɛpɨˈmiːθiːəs 50px 116.2±3.6
(130 × 114 × 106)
526.6±0.6 151422 +0.69433 0.335° 0.0098 co-orbital with Janus 1977 J. Fountain, and S. Larson
7b X Janus Janus ˈdʒeɪnəs 50px 179.0±2.8
(203 × 185 × 153)
1897.5±0.6 151472 +0.69466 0.165° 0.0068 co-orbital with Epimetheus 1966 A. Dollfus
9 LIII Aegaeon Aegaeon iːˈdʒiːən 50px ≈ 0.5 ≈ 0.0001 167500 +0.80812 0.001° 0.0002 G Ring moonlet 2008 Cassini–Huygens
10 I MimasMimas ˈmaɪməs 50px 396.4±0.8
(416 × 393 × 381)
37493±31 185404 +0.942422 1.566° 0.0202   1789 W. Herschel
11 XXXII Methone Methone mɨˈθoʊniː 50px 3.2±1.2 ≈ 0.02 194440 +1.00957 0.007° 0.0001 Alkyonides 2004 Cassini–Huygens
14 XLIX Anthe Anthe ˈænθiː An animated image showing as a dot (right) moves around Saturn (left) outside the main rings (in the middle), which are viewed from a relatively low angle ≈ 1 ≈ 0.007 197700 +1.03650 0.1° 0.001 Alkyonides 2007 Cassini–Huygens
13 XXXIII Pallene Pallene pəˈliːniː 50px 5.0±1.2
(6 × 6 × 4)
≈ 0.05 212280 +1.15375 0.181° 0.0040 Alkyonides 2004 Cassini–Huygens
14 II EnceladusEnceladus ɛnˈsɛlədəs 50px 504.2±0.4
(513 × 503 × 497)
108022±101 237950 +1.370218 0.010° 0.0047 Generates the E ring 1789 W. Herschel
15 III TethysTethys ˈtiːθɨs / ˈtɛθɨs 50px 1062±1.2
(1077 × 1057 × 1053)
617449±132 294619 +1.887802 0.168° 0.0001   1684 G. Cassini
15a XIII Telesto Telesto tɨˈlɛstoʊ A potato shaped body is illuminated from the right. The terminator runs from the top to bottom. There is a large crater at the bottom near the terminator. The body is elongated from the right to left. 24.8±0.8
(33 × 24 × 20)
≈ 9.41 294619 +1.887802 1.158° 0.000 leading Tethys trojan 1980 B. Smith, H. Reitsema, S. Larson, and J. Fountain
15b XIV Calypso Calypso kəˈlɪpsoʊ 50px 21.4±1.4
(30 × 23 × 14)
≈ 6.3 294619 +1.887802 1.473° 0.000 trailing Tethys trojan 1980 D. Pascu, P. Seidelmann, W. Baum, and D. Currie
18 IV DioneDione daɪˈoʊniː 50px 1122.8±0.8
(1128 × 1123 × 1119)
1095452±168 377396 +2.736915 0.002° 0.0022   1684 G. Cassini
18a XII Helene Helene ˈhɛlɨniː 50px 35.2±0.8
(43 × 38 × 26)
≈ 24.46 377396 +2.736915 0.212° 0.0022 leading Dione trojan 1980 P. Laques and J. Lecacheux
18b XXXIV Polydeuces Polydeuces ˌpɒliˈdjuːsiːz 50px 2.6±0.8
(3 × 2 × 1)
≈ 0.03 377396 +2.736915 0.177° 0.0192 trailing Dione trojan 2004 Cassini–Huygens
21 V RheaRhea ˈriːə 50px 1527.0±1.2
(1530 × 1526 × 1525)
2306518±353 527108 +4.518212 0.327° 0.001258   1672 G. Cassini
22 VI TitanTitan ˈtaɪtən 55px 5151 134520000±20000 1221930 +15.94542 0.3485° 0.0288   1655 C. Huygens
23 VII HyperionHyperion haɪˈpɪəriən 50px 270±8
(360 × 266 × 205)
5620±50 1481010 +21.27661 0.568° 0.123006 in 4:3 resonance with Titan 1848 W. Bond
G. Bond
W. Lassell
24 VIII IapetusIapetus aɪˈæpɨtəs 50px 1468.6±5.6
(1491 × 1491 × 1424)
1805635±375 3560820 +79.3215 15.47° 0.028613   1671 G. Cassini
25 XXIV KiviuqKiviuq ˈkɪviək ≈ 16 ≈ 2.79 11294800 +448.16 49.087° 0.3288 Inuit group 2000 B. Gladman, J. Kavelaars, et al.
26 XXII IjiraqIjiraq ˈiː.ɨrɒk ≈ 12 ≈ 1.18 11355316 +451.77 50.212° 0.3161 Inuit group 2000 B. Gladman, J. Kavelaars, et al.
27 IX Phoebe ♣†Phoebe ˈfiːbiː 50px 213.0±1.4
(219 × 217 × 204)
8292±10 12869700 545.09 173.047° 0.156242 Norse group 1899 W. Pickering
28 XX PaaliaqPaaliaq ˈpɑːliɒk ≈ 22 ≈ 7.25 15103400 +692.98 46.151° 0.3631 Inuit group 2000 B. Gladman, J. Kavelaars, et al.
29 XXVII SkathiSkathi ˈskɒði ≈ 8 ≈ 0.35 15672500 732.52 149.084° 0.246 Norse (Skathi) Group 2000 B. Gladman, J. Kavelaars, et al.
30 XXVI AlbiorixAlbiorix ˌælbiˈɒrɪks ≈ 32 ≈ 22.3 16266700 +774.58 38.042° 0.477 Gallic group 2000 M. Holman
31   S/2007AS/2007 S 2 ≈ 6 ≈ 0.15 16560000 792.96 176.68° 0.2418 Norse group 2007 S. Sheppard, D. Jewitt, J. Kleyna, B. Marsden
32 XXXVII BebhionnBebhionn bɛˈviːn, ˈvɪvi.ɒn ≈ 6 ≈ 0.15 17153520 +838.77 40.484° 0.333 Gallic group 2004 S. Sheppard, D. Jewitt, J. Kleyna
33 XXVIII ErriapusErriapus ˌɛriˈæpəs ≈ 10 ≈ 0.68 17236900 +844.89 38.109° 0.4724 Gallic group 2000 B. Gladman, J. Kavelaars, et al.
34 XLVII SkollSkoll ˈskɒl, ˈskɜːl ≈ 6 ≈ 0.15 17473800 862.37 155.624° 0.418 Norse (Skathi) group 2006 S. Sheppard, D. Jewitt, J. Kleyna
35 XXIX SiarnaqSiarnaq ˈsiːɑrnək ≈ 40 ≈ 43.5 17776600 +884.88 45.798° 0.24961 Inuit group 2000 B. Gladman, J. Kavelaars, et al.
36 LII TarqeqTarqeq ˈtɑrkeɪk ≈ 7 ≈ 0.23 17910600 +894.86 49.904° 0.1081 Inuit group 2007 S. Sheppard, D. Jewitt, J. Kleyna
37   S/2004BS/2004 S 13 ≈ 6 ≈ 0.15 18056300 905.85 167.379° 0.261 Norse group 2004 S. Sheppard, D. Jewitt, J. Kleyna
38 LI GreipGreip ˈɡreɪp ≈ 6 ≈ 0.15 18065700 906.56 172.666° 0.3735 Norse group 2006 S. Sheppard, D. Jewitt, J. Kleyna
39 XLIV HyrrokkinHyrrokkin hɪˈrɒkɨn ≈ 8 ≈ 0.35 18168300 914.29 153.272° 0.3604 Norse (Skathi) group 2006 S. Sheppard, D. Jewitt, J. Kleyna
40 L JarnsaxaJarnsaxa jɑrnˈsæksə ≈ 6 ≈ 0.15 18556900 943.78 162.861° 0.1918 Norse group 2006 S. Sheppard, D. Jewitt, J. Kleyna
41 XXI TarvosTarvos ˈtɑrvɵs ≈ 15 ≈ 2.3 18562800 +944.23 34.679° 0.5305 Gallic group 2000 B. Gladman, J. Kavelaars, et al.
42 XXV MundilfariMundilfari ˌmʊndəlˈvɛri ≈ 7 ≈ 0.23 18725800 956.70 169.378° 0.198 Norse group 2000 B. Gladman, J. Kavelaars, et al.
43   S/2006S/2006 S 1 ≈ 6 ≈ 0.15 18930200 972.41 154.232° 0.1303 Norse (Skathi) group 2006 S. Sheppard, D.C. Jewitt, J. Kleyna
44   S/2004CS/2004 S 17 ≈ 4 ≈ 0.05 19099200 985.45 166.881° 0.226 Norse group 2004 S. Sheppard, D. Jewitt, J. Kleyna
45 XXXVIII BergelmirBergelmir bɛərˈjɛlmɪər ≈ 6 ≈ 0.15 19104000 985.83 157.384° 0.152 Norse (Skathi) group 2004 S. Sheppard, D. Jewitt, J. Kleyna
46 XXXI NarviNarvi ˈnɑrvi ≈ 7 ≈ 0.23 19395200 1008.45 137.292° 0.320 Norse (Narvi) group 2003 S. Sheppard, D. Jewitt, J. Kleyna
47 XXIII SuttungrSuttungr ˈsʊtʊŋɡər ≈ 7 ≈ 0.23 19579000 1022.82 174.321° 0.131 Norse group 2000 B. Gladman, J. Kavelaars, et al.
48 XLIII HatiHati ˈhɑːti ≈ 6 ≈ 0.15 19709300 1033.05 163.131° 0.291 Norse group 2004 S. Sheppard, D. Jewitt, J. Kleyna
49   S/2004AS/2004 S 12 ≈ 5 ≈ 0.09 19905900 1048.54 164.042° 0.396 Norse group 2004 S. Sheppard, D. Jewitt, J. Kleyna
50 XL FarbautiFarbauti fɑrˈbaʊti ≈ 5 ≈ 0.09 19984800 1054.78 158.361° 0.209 Norse (Skathi) group 2004 S. Sheppard, D. Jewitt, J. Kleyna
51 XXX ThrymrThrymr ˈθrɪmər ≈ 7 ≈ 0.23 20278100 1078.09 174.524° 0.453 Norse group 2000 B. Gladman, J. Kavelaars, et al.
52 XXXVI AegirAegir ˈaɪ.ɪər ≈ 6 ≈ 0.15 20482900 1094.46 167.425° 0.237 Norse group 2004 S. Sheppard, D. Jewitt, J. Kleyna
53   S/2007BS/2007 S 3 ≈ 5 ≈ 0.09 20518500 ≈ 1100 177.22° 0.130 Norse group 2007 S. Sheppard, D. Jewitt, J. Kleyna
54 XXXIX BestlaBestla ˈbɛstlə ≈ 7 ≈ 0.23 20570000 1101.45 147.395° 0.5145 Norse (Narvi) group 2004 S. Sheppard, D. Jewitt, J. Kleyna
55   S/2007CS/2004 S 7 ≈ 6 ≈ 0.15 20576700 1101.99 165.596° 0.5299 Norse group 2004 S. Sheppard, D. Jewitt, J. Kleyna
56   S/2006S/2006 S 3 ≈ 6 ≈ 0.15 21076300 1142.37 150.817° 0.4710 Norse (Skathi) group 2006 S. Sheppard, D. Jewitt, J. Kleyna
57 XLI FenrirFenrir ˈfɛnrɪər ≈ 4 ≈ 0.05 21930644 1212.53 162.832° 0.131 Norse group 2004 S. Sheppard, D. Jewitt, J. Kleyna
58 XLVIII SurturSurtur ˈsɜrtər ≈ 6 ≈ 0.15 22288916 1242.36 166.918° 0.3680 Norse group 2006 S. Sheppard, D. Jewitt, J. Kleyna
59 XLV KariKari ˈkɑri ≈ 7 ≈ 0.23 22321200 1245.06 148.384° 0.3405 Norse (Skathi) group 2006 S. Sheppard, D. Jewitt, J. Kleyna
60 XIX YmirYmir ˈɪmɪər ≈ 18 ≈ 3.97 22429673 1254.15 172.143° 0.3349 Norse group 2000 B. Gladman, J. Kavelaars, et al.
61 XLVI LogeLoge ˈlɔɪ.eɪ ≈ 6 ≈ 0.15 22984322 1300.95 166.539° 0.1390 Norse group 2006 S. Sheppard, D. Jewitt, J. Kleyna
62 XLII FornjotFornjot ˈfɔrnjɒt ≈ 6 ≈ 0.15 24504879 1432.16 167.886° 0.186 Norse group 2004 S. Sheppard, D. Jewitt, J. Kleyna

Unconfirmed moons

The following objects (observed by Cassini) have not been confirmed as solid bodies. It is not yet clear if these are real satellites or merely persistent clumps within the F Ring.[18]

Name Image Diameter (km) Semi-major
axis (km)[42]
period (d)[42]
Position Discovery year
S/2004 S 6 50px ≈ 3–5 ≈ 140130 +0.61801 uncertain objects around the F Ring 2004
S/2004 S 3/S 4[j] A segment of the ring with bright overexposed Saturn in the top-left corner. Near the right edge of the ring there is a bright dot. ≈ 3–5 ≈ 140300 ≈ +0.619 2004

Hypothetical moons

Two moons were claimed to be discovered by different astronomers but never seen again. Both moons were said to orbit between Titan and Hyperion.[74]


It is thought that the Saturnian system of Titan, mid-sized moons, and rings developed from a set-up closer to the Galilean moons of Jupiter, though the details are unclear. It has been proposed either that a second Titan-sized moon broke up, producing the rings and inner mid-sized moons,[75] or that two large moons fused to form Titan, with the collision scattering icy debris that formed the mid-sized moons.[76] On June 23, 2014, NASA claimed to have strong evidence that nitrogen in the atmosphere of Titan came from materials in the Oort cloud, associated with comets, and not from the materials that formed Saturn in earlier times.[59]


  1. ^ The mass of the rings is about the mass of Mimas,[8] whereas the combined mass of Janus, Hyperion and Phoebe—the most massive of the remaining moons—is about one-third of that. The total mass of the rings and small moons is around 5.5×1019Lua error: Unmatched close-bracket at pattern character 67..
  2. ^ Inktomi was once known as "The Splat".[56]
  3. ^ The photometric color may be used as a proxy for the chemical composition of satellites' surfaces.
  4. ^ A confirmed moon is given a permanent designation by the IAU consisting of a name and a Roman numeral.[30] The nine moons that were known before 1900 (of which Phoebe is the only irregular) are numbered in order of their distance from Saturn; the rest are numbered in the order by which they received their permanent designations. Nine small moons of the Norse group and S/2009 S 1 have not yet received a permanent designation.
  5. ^ The diameters and dimensions of the inner moons from Pan through Janus, Methone, Pallene, Telepso, Calypso, Helene, Hyperion and Phoebe were taken from Thomas 2010, Table 3.[32] Diameters and dimensions of Mimas, Enceladus, Tethys, Dione, Rhea and Iapetus are from Thomas 2010, Table 1.[32] The approximate sizes of other satellites are from the website of Scott Sheppard.[36]
  6. ^ Masses of the large moons were taken from Jacobson, 2006.[33] Masses of Pan, Daphnis, Atlas, Prometheus, Pandora, Epimetheus, Janus, Hyperion and Phoebe were taken from Thomas, 2010, Table 3.[32] Masses of other small moons were calculated assuming a density of 1.3 g/cm3.
  7. ^ a b c The orbital parameters were taken from Spitale, et al. 2006,[42] IAU-MPC Natural Satellites Ephemeris Service,[73] and NASA/NSSDC.[34]
  8. ^ Negative orbital periods indicate a retrograde orbit around Saturn (opposite to the planet's rotation).
  9. ^ To Saturn's equator for the regular satellites, and to the ecliptic for the irregular satellites
  10. ^ S/2004 S 4 was most likely a transient clump—it has not been recovered since the first sighting.[18]


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