Artist's concepts of the Saturnian ring–moon system
A spherical yellow-brownish body (Saturn) can be seen on the left. It is viewed at an oblique angle with respect to its equatorial plane. Around Saturn there are rings and small ring moons. Further to the right large round moons are shown in order of their distance.
Saturn, its rings and major icy moons—from Mimas to Rhea
In the foreground there are six round fully illuminated bodies and some small irregular objects. A large half-illuminated body is shown in the background with circular cloud bands around the partially darkened north pole visible.
Images of several moons of Saturn. From left to right: Mimas, Enceladus, Tethys, Dione, Rhea; Titan in the background; Iapetus (top right) and irregularly shaped Hyperion (bottom right). Some small moons are also shown. All to scale.

The moons of Saturn are numerous and diverse, ranging from tiny moonlets only tens of meters across to the enormous Titan, which is larger than the planet Mercury. There are 83 moons with confirmed orbits as of 2023.[1] This number does not include the many thousands of moonlets embedded within its dense rings, nor hundreds of possible kilometer-sized distant moons that were only briefly captured by telescopes.[2][3][4] Seven Saturnian moons are large enough to have collapsed into a relaxed, ellipsoidal shape, though only one or two of those, Titan and possibly Rhea, are currently in hydrostatic equilibrium. Particularly notable among Saturn's moons are Titan, the second-largest moon in the Solar System (after Jupiter's Ganymede), with a nitrogen-rich Earth-like atmosphere and a landscape featuring dry river networks and hydrocarbon lakes,[5] Enceladus, which emits jets of ice from its south-polar region and is covered in a deep layer of snow,[6] and Iapetus, with its contrasting black and white hemispheres.

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 narrow F Ring. Two other known regular satellites orbit within gaps in Saturn's rings. The relatively large Hyperion is locked in an orbital resonance with Titan. The remaining regular moons orbit near the outer edge of the dense A Ring, within the diffuse 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 fifty-nine, with mean diameters ranging from 2 to 213 km (1 to 132 mi), 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 fragments from the collisional breakup of such bodies after they were captured, creating collisional families. Saturn is expected to have around 150 irregular satellites larger than 2.8 km (1.7 mi) in diameter, plus many hundreds more that are even smaller. The irregular satellites are classified by their orbital characteristics into the Inuit, Norse, and Gallic groups, and their names are chosen from the corresponding mythologies (with the Gallic group corresponding to Celtic mythology). The sole exception is Phoebe, the ninth moon of Saturn and largest irregular, discovered at the end of the 19th century; it is part of the Norse group but named for a Greek Titaness.

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.[3]

There are still twenty unnamed moons (as of November 2022), of which all but one is irregular. If named, they will receive names from Gallic, Norse and Inuit mythology based on the orbital groups of the moons.[9][10]

Discovery

Saturn (overexposed) and the moons Iapetus, Titan, Dione, Hyperion, and Rhea viewed through a 12.5-inch telescope
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 57-millimeter (2.2 in) objective lens[11] on a refracting telescope of his own design.[12] Tethys, Dione, Rhea and Iapetus (the "Sidera Lodoicea") were discovered between 1671 and 1684 by Giovanni Domenico Cassini.[13] Mimas and Enceladus were discovered in 1789 by William Herschel.[13] Hyperion was discovered in 1848 by W. C. Bond, G. P. Bond[14] and William Lassell.[15]

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.[16] In 1966 the tenth satellite of Saturn was discovered by Audouin Dollfus, when the rings were observed edge-on near an equinox.[17] 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.[17] 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.[18] 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).[18]

Observations by spacecraft

Circular complex rings of Saturn are seen at the low angle. The rings look like two grayish bands running parallel to each other from the left to right and connecting at the far right. Half illuminated Titan and Dione are visible slightly below the rings in the foreground. Two bright dots: one at the lower edge of rings and another above the rings can be seen. They are Prometheus and Telepso.
Four moons of Saturn can be seen on this image by the Cassini spacecraft: The larger Titan and Dione at the bottom, small Prometheus (under the rings) and small Telesto above center.
Five moons in another Cassini image: Rhea bisected in the far-right 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.[18] In addition, Epimetheus was confirmed as distinct from Janus. In 1990, Pan was discovered in archival Voyager images.[18]

The Cassini mission,[19] 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 trojan moon of Dione – Polydeuces. It also observed three suspected but unconfirmed moons in the F Ring.[20] 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, had been visually confirmed at the time.[21] In 2007 Anthe was announced.[22] 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.[23] In March 2009, Aegaeon, a moonlet within the G Ring, was announced.[24] In July of the same year, S/2009 S 1, the first moonlet within the B Ring, was observed.[25] In April 2014, the possible beginning of a new moon, within the A Ring, was reported.[26] (related image)

Outer moons

Quadruple Saturn–moon transit captured by the Hubble Space Telescope
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 20th century, Phoebe stood alone among Saturn's known moons with its highly irregular orbit. Then in 2000, three dozen additional irregular moons have been discovered using ground-based telescopes.[27] 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.[28] They are probably fragments of larger bodies captured by Saturn's gravitational pull.[27][28] In 2005, astronomers using the Mauna Kea Observatory announced the discovery of twelve more small outer moons,[29][30] in 2006, astronomers using the Subaru 8.2 m telescope reported the discovery of nine more irregular moons,[31] in April 2007, Tarqeq (S/2007 S 1) was announced and in May of the same year S/2007 S 2 and S/2007 S 3 were reported.[32] In 2019, twenty new irregular satellites of Saturn were reported, resulting in Saturn overtaking Jupiter as the planet with the most known moons for the first time since 2000.[10][2] Yet another was reported in 2021, after a survey for Saturnian moons took place in 2019.[33][34]

The number of moons known for each of the four outer planets up to February 2023. Saturn currently has 83 known satellites.
The number of moons known for each of the four outer planets up to February 2023. Saturn currently has 83 known satellites.

Naming

Main article: Naming of moons

The modern names for Saturnian moons were suggested by John Herschel in 1847.[13] He proposed to name them after mythological figures associated with the Roman titan of time, Saturn (equated to the Greek Cronus).[13] In particular, the then known seven satellites were named after Titans, Titanesses and Giants—brothers and sisters of Cronus.[16] Herschel followed Simon Marius's writings:[35]

As Saturn devoured his children, his family could not be assembled around him, so that the choice lay among his brothers and sister, the Titans and Titanesses. The name Iapetus seemed indicated by the obscurity and remoteness of the exterior satellite, Titan by the superior size of the Huyghenian, while the three female appellations [Rhea, Dione, and Tethys] class together the three intermediate Cassinian satellites. The minute interior ones seemed appropriately characterized by a return to male appellations [Enceladus and Mirnas] chosen from a younger and inferior (though still superhuman) brood. ["Results of the Astronomical Observations made...at the Cape of Good Hope," p. 415]

In 1848, Lassell proposed that the eighth satellite of Saturn be named Hyperion after another Titan.[15][35] 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.[36] All the irregular moons (except Phoebe, discovered about a century before the others) are named after Inuit and Gallic gods and after Norse ice giants.[37]

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, three more asteroids would share the names of Saturnian moons but for spelling differences made permanent by the International Astronomical Union (IAU): Calypso and asteroid 53 Kalypso; Helene and asteroid 101 Helena; and Gunnlod and asteroid 657 Gunlöd.

Sizes

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 small moons, together with the rings, comprise only 0.04%.[a]

The relative masses of Saturn's moons. Values are ×1021 kg. With Titan in the comparison (left), Mimas and Enceladus are invisible at this scale. Even excluding Titan (right), Phoebe, Hyperion, the smaller moons and the rings are invisible.
Saturn's major satellites, compared to the Moon
Name
 Diameter
(km)[38] 		Mass
(kg)[39] 		Orbital radius
(km)[40] 		Orbital period
(days)[40]
Mimas 396
(0.12 D☾)		 4×1019
(0.0005 M☾)		 185,539
(0.48 a☾)		 0.9
(0.03 T☾)
Enceladus 504
(0.14 D☾)		 1.1×1020
(0.002 M☾)		 237,948
(0.62 a☾)		 1.4
(0.05 T☾)
Tethys 1,062
(0.30 D☾)		 6.2×1020
(0.008 M☾)		 294,619
(0.77 a☾)		 1.9
(0.07 T☾)
Dione 1,123
(0.32 D☾)		 1.1×1021
(0.015 M☾)		 377,396
(0.98 a☾)		 2.7
(0.10 T☾)
Rhea 1,527
(0.44 D☾)		 2.3×1021
(0.03 M☾)		 527,108
(1.37 a☾)		 4.5
(0.20 T☾)
Titan 5,149
(1.48 D☾)
(0.75 D♂)		 1.35×1023
(1.80 M☾)
(0.21 M♂)		 1,221,870
(3.18 a☾)		 16
(0.60 T☾)
Iapetus 1,470
(0.42 D☾)		 1.8×1021
(0.025 M☾)		 3,560,820
(9.26 a☾)		 79
(2.90 T☾)

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.[41] 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.[2] 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.[37]

Ring moonlets

Main article: Rings of Saturn § Moonlet
Saturn's F Ring along with the moons, Enceladus and Rhea
Sequence of Cassini images of Aegaeon embedded within the bright arc of Saturn's G Ring

During late July 2009, a moonlet, S/2009 S 1, was discovered in the B Ring, 480 km from the outer edge of the ring, by the shadow it cast.[25] 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.[42]

In 2006, four tiny moonlets were found in Cassini images of the A Ring.[43] 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.[43] 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.[44] The moonlets themselves are tiny, ranging from about 40 to 500 meters in diameter, and are too small to be seen directly.[3]

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

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.[3] This region is relatively free from the disturbances caused by resonances with larger satellites,[3] 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.[44] 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.[3] In April 2014, NASA scientists reported the possible consolidation of a new moon within the A Ring, implying that Saturn's present moons may have formed in a similar process in the past when Saturn's ring system was much more massive.[26]

Similar moonlets may reside in the F Ring.[3] 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.[45]

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.[24] 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.[46]

Ring shepherds

Main article: Rings of Saturn
Shepherd moon Daphnis in the Keeler gap
Shepherd moon Daphnis in the Keeler gap
Shepherd moons Atlas, Daphnis and Pan (enhanced color). They bear distinct equatorial ridges that appear to have formed from material accreted from Saturn's rings.
Shepherd moons Atlas, Daphnis and Pan (enhanced color). They bear distinct equatorial ridges that appear to have formed from material accreted from Saturn's rings.

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).[20][24] 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.[41]

Co-orbitals

Main article: Co-orbital moon

Janus and Epimetheus are called co-orbital moons.[18] They are of roughly equal size, with Janus being slightly larger than Epimetheus.[41] 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, their gravitational interaction causes them to swap orbits every four years.[47]

Inner large

South pole map of tiger stripes on Enceladus
South pole map of tiger stripes on Enceladus
Saturn's rings and moons
Saturn's moons from bottom to top: Mimas, Enceladus, and Tethys
Tethys and the rings of Saturn
Color view of Dione in front of Saturn

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

Alkyonides

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 have very faint ring arcs along their orbits, whereas Pallene has a faint complete ring.[54] Of these three moons, only Methone has been photographed at close range, showing it to be egg-shaped with very few or no craters.[55]

Trojan

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).[20] Helene is by far the largest trojan moon,[48] while Polydeuces is the smallest and has the most chaotic orbit.[47] These moons are coated with dusty material that has smoothed out their surfaces.[56]

Outer large

Saturn's outer moons
A spherical body is almost fully illuminated. Its grayish surface is covered by numerous circular craters. The terminator is located near the upper-right limb. A large crater can be seen near the limb in the upper-left part of the body. Another smaller bright crater can be seen in the center. It is surrounded by a large bright patch having the shape of a five-pointed star.
Inktomi or "The Splat", a relatively young crater with prominent butterfly-shaped ejecta on Rhea's leading hemisphere
Titan in front of Dione and the rings of Saturn
An irregularly-shaped and heavily cratered body, pock-marked with dark pits and ridges on its tan-colored icy surface.
Cassini image of Hyperion
A part of a spherical body illuminated from the above and behind. The convex limb runs from the lower-left to the upper-right corner. The black outer space is in the upper-left corner. The terminator is near the bottom. The surface of the body is covered with numerous craters. A large ridge runs in the center from the top to bottom.
Equatorial ridge on Iapetus

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

Irregular

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.
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.
Orbits and positions of Saturn's irregular moons as of 1 January 2021. Prograde orbits are colored blue while retrograde orbits are colored red.
Orbits and positions of Saturn's irregular moons as of 1 January 2021. Prograde orbits are colored blue while retrograde orbits are colored red.

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.[27] 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.[28] The irregulars generally have featureless visible and near infrared spectra dominated by water absorption bands.[27] They are neutral or moderately red in color—similar to C-type, P-type, or D-type asteroids,[37] though they are much less red than Kuiper belt objects.[27][c]

Inuit

Main article: Inuit group

The Inuit group includes eight 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.[28][37] The moons are Ijiraq, Kiviuq, Paaliaq, Siarnaq, and Tarqeq,[37] along with three unnamed moons Saturn LX, S/2004 S 31, and S/2019 S 1. The largest among them is Siarnaq with an estimated size of about 40 km.

Gallic

Main article: 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.[28][37] They are Albiorix, Bebhionn, Erriapus, and Tarvos.[37] The largest among these moons is Albiorix with an estimated size of about 32 km. There is an additional satellite S/2004 S 24 that could belong to this group, but more observations are needed to confirm or disprove its categorization. S/2004 S 24 has the most distant prograde orbit of Saturn's known satellites.

Norse

Main article: Norse group

All 46 retrograde outer moons of Saturn are broadly classified into the Norse group.[28][37] They are Aegir, Angrboda, Alvaldi, Beli, Bergelmir, Bestla, Eggther, Farbauti, Fenrir, Fornjot, Geirrod, Gerd, Greip, Gridr, Gunnlod, Hati, Hyrrokkin, Jarnsaxa, Kari, Loge, Mundilfari, Narvi, Phoebe, Skathi, Skoll, Skrymir, Surtur, Suttungr, Thiazzi, Thrymr, Ymir,[37] and fifteen unnamed satellites. 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, with the most apparent being the Phoebe subgroup at inclinations around 175°.[37][4]

List

Orbital diagram of the orbital inclination and orbital distances for Saturn's rings and moon system at various scales. Notable moons, moon groups, and rings are individually labeled. Open the image for full resolution.
Orbital diagram of the orbital inclination and orbital distances for Saturn's rings and moon system at various scales. Notable moons, moon groups, and rings are individually labeled. Open the image for full resolution.

Confirmed

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 and marked with a blue background, while the irregular moons are listed in red, orange and gray background. The orbits and mean distances of the irregular moons are strongly variable over short timescales due to frequent planetary and solar perturbations, therefore the listed orbital elements of all irregular moons are averaged over a 300-year numerical integration. Their orbital elements are all based on the epoch of 1 January 2000.[79]

Key
♠
Titan 		†
Other round moons 		 
Small regular moons 		‡
Inuit group 		♦
Gallic group 		♣
Norse group
Label
[d] 		Name Pronunciation Image Abs.
magn.[80] 		Diameter
(km)[e] 		Mass
(×1015 kg)[f] 		Semi-major
axis
(km)[g] 		Orbital period (d)[g][h] Inclination
(°)[g][i] 		Eccentricity Position Discovery
year[1] 		Year announced Discoverer[36][1]
S/2009 S 1 —
PIA11665 moonlet in B Ring cropped.jpg
— 0.30 < 0.00000001 ≈ 117000 ≈ 0.47150 ≈ 0.000 ≈ 0.0000 outer B Ring 2009 2009 Cassini[25]
(moonlets) —
A noisy image showing a few bright dots marked by circles
— 0.04–0.4 < 0.00000002 ≈ 130000 ≈ 0.55 ≈ 0.000 ≈ 0.0000 Three 1,000 km bands within A Ring[3] 2006 — Cassini
XVIII Pan /ˈpæn/
An irregularly shaped body with a prominent equatorial ridge. It is illuminated from the bottom right.
9.1 28.2
(34 × 31 × 20)		 5.0 133584 +0.57505 0.000 0.0000 in Encke Division 1990 1990 Showalter
XXXV Daphnis /ˈdæfnəs/
A small, irregularly shaped body elongated from the bottom left to top right. It is illuminated from the bottom left.
12.0 28.2
(8.6 × 8.2 × 6.4)		 0.077 136505 +0.59408 0.004 0.0000 in Keeler Gap 2005 2005 Cassini
XV Atlas /ˈætləs/
An irregularly shaped body is fully illuminated. The body, which looks like a cone viewed from the south pole, is elongated downward.
10.7 30.2
(41 × 35 × 19)		 6.6 137670 +0.60169 0.003 0.0012 outer A Ring shepherd 1980 1980 Voyager 1
XVI Prometheus /proʊˈmiːθiəs/
An irregularly shaped oblong body is fully illuminated. It is elongated in the direction from the top left to bottom left. Its surface is covered by craters.
6.5 86.2
(136 × 79 × 59)		 159.5 139380 +0.61299 0.008 0.0022 inner F Ring shepherd 1980 1980 Voyager 1
XVII Pandora /pænˈdɔːrə/
An irregularly shaped body is half illuminated from the bottom. The terminator runs from the left to right. The surface is covered by numerous craters.
6.6 81.4
(104 × 81 × 64)		 137.1 141720 +0.62850 0.050 0.0042 outer F Ring shepherd 1980 1980 Voyager 1
XI Epimetheus /ɛpəˈmiːθiəs/
A partially-illuminated irregular body, which has a shape remotely resembling a cube. The body
5.6 116.2
(130 × 114 × 106)		 526.6 151422 +0.69433 0.335 0.0098 co-orbital with Janus 1966 1967 Fountain & Larson
X Janus /ˈdʒeɪnəs/
An irregular body, whose outline looks like an approximate circle in this image. It is illuminated from the bottom-left. The terminator runs from the top-left to bottom-right. The surface is covered by craters.
4.7 179.0
(203 × 185 × 153)		 1897.5 151472 +0.69466 0.165 0.0068 co-orbital with Epimetheus 1966 1967 Dollfus
LIII Aegaeon /iːˈdʒiːɒn/
Image of Aegaeon by Cassini.
18.7 0.66
(1.4 × 0.5 × 0.4)		 ≈ 0.000073 167500 +0.80812 0.001 0.0004 G Ring moonlet 2008 2009 Cassini
I †Mimas /ˈmaɪməs/
A spherical body is half illuminated from the left. The terminator runs from the top to bottom in the vicinity of the right limb. A large crater with a central peak sits on the terminator slightly to the right and above the center of the body. It makes the body look like the Death Star. There are numerous smaller craters.
2.7 396.4
(416 × 393 × 381)		 37493 185404 +0.94242 1.566 0.0202   1789 1789 Herschel
XXXII Methone /məˈθoʊniː/
A smooth, featureless ellipsoidal object illuminated from the top right, distinctly looking like an egg.
13.8 2.9
(3.9 × 2.6 × 2.4)		 ≈ 0.0063 194440 +1.00957 0.007 0.0001 Alkyonides 2004 2004 Cassini
XLIX Anthe /ˈænθiː/
A blurry ellipsoidal object in the center of the image
14.8 1.0 ≈ 0.00026 197700 +1.05089 0.100 0.0011 Alkyonides 2007 2007 Cassini
XXXIII Pallene /pəˈliːniː/
A small, half-illuminated ellipsoidal object in front of Saturn as a backdrop
12.9 4.4
(5.8 × 4.2 × 3.7)		 ≈ 0.023 212280 +1.15375 0.181 0.0040 Alkyonides 2004 2004 Cassini
II †Enceladus /ɛnˈsɛlədəs/
PIA17202 - Approaching Enceladus.jpg
1.8 504.2
(513 × 503 × 497)		 108022 237950 +1.37022 0.010 0.0047 Generates the E ring 1789 1789 Herschel
III †Tethys /ˈtiːθəs/
Tethys.jpg.fromcassini.jpg
0.3 1062.2
(1077 × 1057 × 1053)		 617449 294619 +1.88780 0.168 0.0001   1684 1684 Cassini
XIII Telesto /təˈlɛstoʊ/
An oblong object with a few large craters and a smooth surface
8.7 24.8
(33 × 24 × 20)		 ≈ 4.0 294619 +1.88780 1.158 0.0010 leading Tethys trojan (L4) 1980 1980 Smith et al.
XIV Calypso /kəˈlɪpsoʊ/
An oblong body is seen in this low resolution image.
8.7 21.4
(30 × 23 × 14)		 ≈ 2.5 294619 +1.88780 1.473 0.0010 trailing Tethys trojan (L5) 1980 1980 Pascu et al.
IV †Dione /daɪˈoʊniː/
Dione in natural light (cropped).jpg
0.4 1122.8
(1128 × 1123 × 1119)		 1095452 377396 +2.73692 0.002 0.0022   1684 1684 Cassini
XII Helene /ˈhɛləniː/
An irregularly shaped body illuminated from the left. Its surface is covered by numerous impact craters.
7.3 35.2
(43 × 38 × 26)		 ≈ 7.2 377396 +2.73692 0.199 0.0022 leading Dione trojan (L4) 1980 1980 Laques & Lecacheux
XXXIV Polydeuces /pɒliˈdjuːsiːz/
A small oblong body is barely resolved in this image.
13.5 2.6
(3.0 × 2.4 × 1.0)		 ≈ 0.0038 377396 +2.73692 0.177 0.0192 trailing Dione trojan (L5) 2004 2004 Cassini
V †Rhea /ˈreɪə/
Rhea true color.jpg
–0.2 1527.6
(1530 × 1526 × 1525)		 2306518 527108 +4.51821 0.327 0.0013   1672 1673 Cassini
VI ♠Titan /ˈtaɪtən/
Titan in true color.jpg
–1.3 5149.46
(5149 × 5149 × 5150)		 134520000 1221930 +15.9454 0.349 0.0288   1655 1656 Huygens
VII Hyperion /haɪˈpɪəriən/
An irregularly shaped oblong body is illuminated from the left. The terminator is near the right limb. The body is elongated in the top-bottom direction. The surface is punctured by numerous impact craters, which make it look like a sponge or cheese.
4.8 270.0
(360 × 266 × 205)		 5619.9 1481010 +21.2766 0.568 0.1230 in 4:3 resonance with Titan 1848 1848 Bond & Lassell
VIII †Iapetus /aɪˈæpətəs/
Iapetus.jpg
1.7 1468.6
(1491 × 1491 × 1424)		 1805635 3560820 +79.3215 15.47 0.0286   1671 1673 Cassini
‡S/2019 S 1 — 15.3 ≈ 3 ≈ 0.014 11244000 +445.60 46.7 0.541 Inuit group 2019 2021 Ashton et al.
XXIV ‡Kiviuq /ˈkɪviək/
Kiviuq-CFHT.gif
12.6 ≈ 16 ≈ 2.1 11307300 +449.13 48.9 0.182 Inuit group 2000 2000 Gladman et al.
XXII ‡Ijiraq /ˈiːɪrɒk/
Ijiraq-discovery-CFHT.gif
13.2 ≈ 12 ≈ 0.90 11344600 +451.46 49.2 0.353 Inuit group 2000 2000 Gladman et al.
IX ♣Phoebe /ˈfiːbi/
An approximately spherical heavily cratered body is illuminated from the bottom-right. The terminator runs near the left and top limbs. There is huge crater at the top, which affects the shape, and another slightly smaller at the bottom.
6.7 213.0
(219 × 217 × 204)		 8292.0 12929400 −550.30 175.2 0.164 Norse group (Phoebe) 1898 1899 Pickering
XX ‡Paaliaq /ˈpɑːliɒk/
Paaliaq-CFHT.gif
11.9 ≈ 22 ≈ 5.6 14997300 +687.08 47.1 0.384 Inuit group 2000 2000 Gladman et al.
XXVII ♣Skathi /ˈskɑːði/
Skathi-discovery-CFHT.gif
14.4 ≈ 8 ≈ 0.27 15575100 −728.10 149.7 0.265 Norse group 2000 2000 Gladman et al.
♣S/2007 S 2 — 15.6 ≈ 4 ≈ 0.034 15939700 −754.90 175.6 0.232 Norse group (Phoebe) 2007 2007 Sheppard et al.
♣S/2004 S 37 — 15.9 ≈ 4 ≈ 0.034 15940500 −754.47 159.3 0.446 Norse group 2004 2019 Sheppard et al.
XXVI ♦Albiorix /ˌælbiˈɒrɪks/
Albiorix WISE-W4.jpg
11.2 28.6 ≈ 12.2 16329100 +783.49 38.9 0.470 Gallic group 2000 2000 Holman
XXXVII ♦Bebhionn /ˈbeɪvɪn/
Bebhionn-cassini.png
15.0 ≈ 6 ≈ 0.11 17028900 +834.94 37.4 0.482 Gallic group 2004 2005 Sheppard et al.
LX ‡S/2004 S 29 — 15.8 ≈ 4 ≈ 0.034 17063900 +837.78 38.6 0.485 Inuit group 2004 2019 Sheppard et al.
‡S/2004 S 31 — 15.6 ≈ 4 ≈ 0.034 17495400 +866.23 48.3 0.202 Inuit group 2004 2019 Sheppard et al.
XXVIII ♦Erriapus /ɛriˈæpəs/
Erriapus-discovery-CFHT.gif
13.7 ≈ 10 ≈ 0.52 17507200 +871.10 38.7 0.462 Gallic group 2000 2000 Gladman et al.
XLVII ♣Skoll /ˈskɒl/ 15.4 ≈ 6 ≈ 0.11 17625700 −878.44 158.4 0.470 Norse group 2006 2006 Sheppard et al.
LII ‡Tarqeq /ˈtɑːrkeɪk/
Tarqeq-cassini.png
14.8 ≈ 7 ≈ 0.18 17748200 +884.98 49.7 0.119 Inuit group 2007 2007 Sheppard et al.
XXIX ‡Siarnaq /ˈsiːɑːrnək/
Siarnaq-discovery-CFHT.gif
10.6 39.3 ≈ 31.8 17880800 +895.87 48.2 0.311 Inuit group 2000 2000 Gladman et al.
XXI ♦Tarvos /ˈtɑːrvəs/
Tarvos discovery.gif
12.9 ≈ 15 ≈ 1.8 18215100 +926.37 38.6 0.528 Gallic group 2000 2000 Gladman et al.
XLIV ♣Hyrrokkin /hɪˈrɒkən/
Hyrrokkin-cassini.png
14.3 ≈ 8 ≈ 0.27 18342600 −931.89 150.3 0.331 Norse group 2004 2005 Sheppard et al.
LI ♣Greip /ˈɡreɪp/
Greip-cassini.png
15.4 ≈ 6 ≈ 0.11 18424000 −936.9 174.3 0.317 Norse group (Phoebe) 2006 2006 Sheppard et al.
♣S/2004 S 13 — 16.3 ≈ 3 ≈ 0.014 18455800 −942.59 168.9 0.266 Norse group 2004 2005 Sheppard et al.
XXV ♣Mundilfari /mʊndəlˈværi/
Mundilfari-discovery-CFHT.gif
 14.5 ≈ 7 ≈ 0.18 18590300 −952.95 168.4 0.210 Norse group 2000 2000 Gladman et al.
♣S/2006 S 1 — 15.6 ≈ 5 ≈ 0.065 18745600 −964.15 155.2 0.105 Norse group 2006 2006 Sheppard et al.
LIV ♣Gridr /ˈɡriːðər/ 15.7 ≈ 4 ≈ 0.034 19250700 −1004.75 163.9 0.187 Norse group 2004 2019 Sheppard et al.
XXXVIII ♣Bergelmir /bɛərˈjɛlmɪər/
Bergelmir.png
15.2 ≈ 6 ≈ 0.11 19269100 −1005.58 158.7 0.144 Norse group 2004 2005 Sheppard et al.
L ♣Jarnsaxa /jɑːrnˈsæksə/ 15.6 ≈ 6 ≈ 0.11 19279700 −1006.92 163.0 0.219 Norse group 2006 2006 Sheppard et al.
XXXI ♣Narvi /ˈnɑːrvi/
Narvi.jpg
14.5 ≈ 7 ≈ 0.18 19286500 −1003.84 143.7 0.449 Norse group 2003 2003 Sheppard et al.
XXIII ♣Suttungr /ˈsʊtʊŋɡər/
Suttungr-discovery-CFHT.gif
14.6 ≈ 7 ≈ 0.18 19391700 −1016.71 175.0 0.116 Norse group (Phoebe) 2000 2000 Gladman et al.
♣S/2004 S 17 — 16.0 ≈ 3 ≈ 0.014 19408100 −1017.49 167.9 0.179 Norse group 2004 2005 Sheppard et al.
♣S/2007 S 3 — 15.7 ≈ 5 ≈ 0.065 19513700 −1026.35 175.6 0.162 Norse group (Phoebe) 2007 2007 Sheppard et al.
XLIII ♣Hati /ˈhɑːti/
Hati-cassini.png
15.4 ≈ 6 ≈ 0.11 19697100 −1040.29 164.1 0.375 Norse group 2004 2005 Sheppard et al.
♣S/2004 S 12 — 15.9 ≈ 4 ≈ 0.034 19770700 −1046.13 163.0 0.325 Norse group 2004 2005 Sheppard et al.
LIX ♣Eggther /ˈɛɡθɛər/ 15.4 ≈ 4 ≈ 0.034 19844700 −1052.33 165.0 0.157 Norse group 2004 2019 Sheppard et al.
XL ♣Farbauti /fɑːrˈbaʊti/ 15.8 ≈ 5 ≈ 0.065 20292500 −1087.29 157.7 0.248 Norse group 2004 2005 Sheppard et al.
XXX ♣Thrymr /ˈθrɪmər/
Thrymr-discovery-CFHT.gif
14.3 ≈ 7 ≈ 0.18 20326500 −1091.84 174.8 0.467 Norse group (Phoebe) 2000 2000 Gladman et al.
XXXIX ♣Bestla /ˈbɛstlə/
Bestla-cassini.png
14.6 ≈ 7 ≈ 0.18 20337900 −1087.46 136.3 0.461 Norse group 2004 2005 Sheppard et al.
♣S/2004 S 7 — 15.6 ≈ 5 ≈ 0.065 20435200 −1100.04 163.3 0.462 Norse group 2004 2005 Sheppard et al.
LV ♣Angrboda /ˈɑːŋɡərboʊðə/ 16.1 ≈ 3 ≈ 0.014 20591000 −1114.05 177.4 0.216 Norse group (Phoebe) 2004 2019 Sheppard et al.
XXXVI ♣Aegir /ˈaɪ.ɪər/ 15.5 ≈ 6 ≈ 0.11 20664600 −1119.33 166.9 0.255 Norse group 2004 2005 Sheppard et al.
LXI ♣Beli /ˈbiːli/ 16.1 ≈ 3 ≈ 0.014 20703800 −1121.76 158.9 0.087 Norse group 2004 2019 Sheppard et al.
LVII ♣Gerd /ˈjɛərð/ 15.7 ≈ 3 ≈ 0.014 20947500 −1142.97 174.4 0.517 Norse group (Phoebe) 2004 2019 Sheppard et al.
LXII ♣Gunnlod /ˈɡʊnlɒð/ 15.5 ≈ 4 ≈ 0.034 21141900 −1157.98 160.4 0.251 Norse group 2004 2019 Sheppard et al.
♣S/2006 S 3 — 15.5 ≈ 5 ≈ 0.065 21352700 −1174.74 157.3 0.443 Norse group 2006 2006 Sheppard et al.
LVI ♣Skrymir /ˈskrɪmɪər/ 15.6 ≈ 4 ≈ 0.034 21448000 −1185.15 175.6 0.437 Norse group (Phoebe) 2004 2019 Sheppard et al.
♣S/2004 S 28 — 15.8 ≈ 4 ≈ 0.034 21867800 −1220.84 169.4 0.160 Norse group 2004 2019 Sheppard et al.
LXV ♣Alvaldi /ɔːlˈvɔːldi/ 15.5 ≈ 4 ≈ 0.034 21995600 −1232.19 177.4 0.238 Norse group (Phoebe) 2004 2019 Sheppard et al.
XLV ♣Kari /ˈkɑːri/
Kari-cassini.png
14.5 ≈ 7 ≈ 0.18 22029700 −1231.01 153.0 0.482 Norse group 2006 2006 Sheppard et al.
LXVI ♣Geirrod /ˈjeɪrɒd/ 15.8 ≈ 4 ≈ 0.034 22259500 −1251.14 154.4 0.539 Norse group 2004 2019 Sheppard et al.
XLI ♣Fenrir /ˈfɛnrɪər/ 15.9 ≈ 4 ≈ 0.034 22331800 −1260.25 164.3 0.136 Norse group 2004 2005 Sheppard et al.
XLVIII ♣Surtur /ˈsɜːrtər/ 15.8 ≈ 6 ≈ 0.11 22753800 −1296.49 168.3 0.449 Norse group 2006 2006 Sheppard et al.
XLVI ♣Loge /ˈlɔɪ.eɪ/
Loge N00177425.jpg
15.3 ≈ 6 ≈ 0.11 22918300 −1311.83 166.9 0.192 Norse group 2006 2006 Sheppard et al.
XIX ♣Ymir /ˈiːmɪər/
Ymir-CFHT.gif
12.3 ≈ 18 ≈ 3.1 22957100 −1315.16 173.1 0.337 Norse group (Phoebe) 2000 2000 Gladman et al.
♣S/2004 S 21 — 16.3 ≈ 3 ≈ 0.014 23125000 −1325.32 155.0 0.409 Norse group 2004 2019 Sheppard et al.
♣S/2004 S 39 — 16.3 ≈ 2 ≈ 0.0042 23195400 −1336.16 167.1 0.102 Norse group 2004 2019 Sheppard et al.
♦S/2004 S 24 — 16.0 ≈ 3 ≈ 0.014 23339900 +1341.25 36.5 0.072 Gallic group?[j] 2004 2019 Sheppard et al.
♣S/2004 S 36 — 16.1 ≈ 3 ≈ 0.014 23433600 −1353.23 152.5 0.617 Norse group[k] 2004 2019 Sheppard et al.
LXIII ♣Thiazzi /θiˈætsi/ 15.9 ≈ 4 ≈ 0.034 23577500 −1366.68 158.8 0.511 Norse group 2004 2019 Sheppard et al.
LXIV ♣S/2004 S 34 — 16.1 ≈ 3 ≈ 0.014 24145500 −1420.77 168.3 0.279 Norse group 2004 2019 Sheppard et al.
XLII ♣Fornjot /ˈfɔːrnjɒt/
Fornjot-cassini.png
15.1 ≈ 6 ≈ 0.11 24937300 −1494.03 169.5 0.214 Norse group 2004 2005 Sheppard et al.
LVIII ♣S/2004 S 26 — 15.7 ≈ 4 ≈ 0.034 26097100 −1603.95 172.9 0.148 Norse group 2004 2019 Sheppard et al.

Unconfirmed

These F Ring moonlets listed in the following table (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.[20]

Name Image Diameter (km) Semi-major
axis (km)[47] 		Orbital
period (d)[47] 		Position Discovery year Status
S/2004 S 3 and S 4[l]
S2004 S 3 - PIA06115.png
≈ 3–5 ≈ 140300 ≈ +0.619 uncertain objects around the F Ring 2004 Were undetected in thorough imaging of the region in November 2004, making their existence improbable
S/2004 S 6
A bright narrow band runs from the top to bottom. To the right of it in the diffuse halo the is a bright small object.
≈ 3–5 ≈ 140130 +0.61801 2004 Consistently detected into 2005, may be surrounded by fine dust and have a very small physical core

In August 2021, researchers Edward Ashton, Brett Gladman, and Matthew Beaudoin identified 120 irregular moons of Saturn, 80 of which are unknown, in an analysis of images taken in July 2019 by the CFHT.[4] All of these candidates were small and faint, with diameters over 3 km (2 mi) at apparent magnitudes of 25–26. Although the researchers consider these candidates very likely irregular moons of Saturn, they all remain unconfirmed due to insufficient observation data for determining reliable orbits.[4] Nevertheless, they found that these Saturnian irregular moon candidates were more abundant at smaller sizes, suggesting that they were likely fragments from a collision that occurred a few hundred million years ago. The researchers extrapolated that the true population of Saturnian irregular moons larger than 2.8 km (2 mi) in diameter amounts to 150±30, which is approximately three times as many Jovian irregular moons down to the same size. If this size distribution applies to even smaller diameters, Saturn would therefore intrinsically have more irregular moons than Jupiter.[4]

Spurious

Two moons were claimed to be discovered by different astronomers but never seen again. Both moons were said to orbit between Titan and Hyperion.[81]

Hypothetical

In 2022, scientists of the Massachusetts Institute of Technology proposed the hypothetical former moon Chrysalis, using data from the Cassini–Huygens mission. Chrysalis would have orbited between Titan and Iapetus, but its orbit would have gradually become more eccentric until it was torn apart by Saturn. 99% of its mass would have been absorbed by Saturn, while the remaining 1% would have formed Saturn's rings.[82][83]

Temporary

Much like Jupiter, asteroids and comets will infrequently make close approaches to Saturn, even more infrequently becoming captured into orbit of the planet. The comet P/2020 F1 (Leonard) is calculated to have made a close approach of 978000±65000 km (608000±40000 mi) to Saturn on 8 May 1936, closer than the orbit of Titan to the planet, with an orbital eccentricity of only 1.098±0.007. The comet may have been orbiting Saturn prior to this as a temporary satellite, but difficulty modelling the non-gravitational forces makes whether or not it was indeed a temporary satellite uncertain.[84]

Other comets and asteroids may have temporarily orbited Saturn at some point, but none are presently known to have.

Formation

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,[85] or that two large moons fused to form Titan, with the collision scattering icy debris that formed the mid-sized moons.[86] On 23 June 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.[65] Studies based on Enceladus's tidal-based geologic activity and the lack of evidence of extensive past resonances in Tethys, Dione, and Rhea's orbits suggest that the moons up to and including Rhea may be only 100 million years old.[87]

See also

Notes

  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 5.5×1019 kg.
  2. ^ Inktomi was once known as "The Splat".[61]
  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.[36] The eight moons that were known before 1850 are numbered in order of their distance from Saturn; the rest are numbered in the order by which they received their permanent designations. Many small moons 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.[38] Diameters and dimensions of Mimas, Enceladus, Tethys, Dione, Rhea and Iapetus are from Thomas 2010, Table 1.[38] The approximate sizes of other satellites are from the website of Scott Sheppard.[2]
  6. ^ Masses of the large moons were taken from Jacobson, 2006.[39] Masses of Pan, Daphnis, Atlas, Prometheus, Pandora, Epimetheus, Janus, Hyperion and Phoebe were taken from Thomas, 2010, Table 3.[38] Masses of small regular satellites were calculated assuming a density of 0.5 g/cm3, while masses of irregular satellites were calculated assuming a density of 1.0 g/cm3.
  7. ^ a b c The orbital parameters were taken from Spitale et al. 2006,[47] IAU-MPC Natural Satellites Ephemeris Service,[80] JPL Solar System Dynamics,[79] and NASA/NSSDC.[40]
  8. ^ Negative orbital periods indicate a retrograde orbit around Saturn (opposite to the planet's rotation). Orbital periods of irregular satellites may not be consistent with their semi-major axes due to perturbations.
  9. ^ To Saturn's equator for the regular satellites, and to the ecliptic for the irregular satellites.
  10. ^ Only known prograde outer satellite, inclination similar to other satellites of the Gallic group
  11. ^ Probably a captured asteroid due to its unusually high eccentricity, though orbit is similar to the Norse group
  12. ^ S/2004 S 4 was most likely a transient clump—it has not been recovered since the first sighting.[20]

References

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