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Moons of Saturn

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An annotated picture of Saturn's many moons captured by the Cassini spacecraft. Shown in the image are Dione, Enceladus, Epimetheus, Prometheus, Mimas, Rhea, Janus, Tethys and Titan.

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 146 moons with confirmed orbits, the most of any planet in the solar system.[1][a] This number does not include the many thousands of moonlets embedded within Saturn's dense rings, nor hundreds of possible kilometer-sized distant moons that have been observed on single occasions.[3][4][5] 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. Three moons are particularly notable. Titan is the second-largest moon in the Solar System (after Jupiter's Ganymede), with a nitrogen-rich Earth-like atmosphere and a landscape featuring river networks and hydrocarbon lakes.[6] Enceladus emits jets of ice from its south-polar region and is covered in a deep layer of snow.[7] Iapetus has contrasting black and white hemispheres as well as an extensive ridge of equatorial mountains among the tallest in the solar system.

Of the known moons, 24 are regular satellites; they have prograde orbits not greatly inclined to Saturn's equatorial plane,[8] with the exception of Iapetus which has a prograde but highly inclined orbit,[9][10] an unusual characteristic for a regular moon. They include the seven major satellites, four small moons that exist in a trojan orbit with larger moons, and five that act as shepherd moons, of which two are mutually co-orbital. Two tiny moons orbit inside of Saturn's B and G rings. The relatively large Hyperion is locked in an orbital resonance with Titan. The remaining regular moons orbit near the outer edges of the dense A Ring and the narrow F 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 122, with mean diameters ranging from 2 to 213 km (1 to 132 mi), orbit much farther from Saturn. They are irregular satellites, having high orbital inclinations and eccentricities 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 prograde Inuit and Gallic groups and the large retrograde Norse group, and their names are chosen from the corresponding mythologies (with the Gallic group corresponding to Celtic mythology). The sole exception is Phoebe, the largest irregular Saturnian moon, 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.[11] Thus an absolute number of Saturnian moons cannot be given, because there is no consensus on a boundary between the countless small unnamed 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.[4]

As of May 2023, there are 83 designated moons that are still unnamed; all but one (the designated B-ring moonlet S/2009 S 1) are irregular. (There are many other undesignated ring moonlets.) If named, most of the irregulars will receive names from Gallic, Norse and Inuit mythology based on the orbital group of which they are a member.[12][13]

Discovery

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A large bright circle in the center is surrounded by small circles.
Saturn (overexposed) and the moons Iapetus, Titan, Dione, Hyperion, and Rhea viewed through a 12.5-inch telescope

Early observations

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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[14] on a refracting telescope of his own design.[15] Tethys, Dione, Rhea and Iapetus (the "Sidera Lodoicea") were discovered between 1671 and 1684 by Giovanni Domenico Cassini.[16] Mimas and Enceladus were discovered in 1789 by William Herschel.[16] Hyperion was discovered in 1848 by W. C. Bond, G. P. Bond[17] and William Lassell.[18]

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.[19] In 1966 the tenth satellite of Saturn was discovered by Audouin Dollfus, when the rings were observed edge-on near an equinox.[20] 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.[20] 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.[21] 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).[21]

Observations by spacecraft

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Five moons in a 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 uncrewed 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.[21] In addition, Epimetheus was confirmed as distinct from Janus. In 1990, Pan was discovered in archival Voyager images.[21]

The Cassini mission,[22] which arrived at Saturn in July 2004, initially discovered three small inner moons: Methone and Pallene between Mimas and Enceladus, and the second trojan moon of Dione, Polydeuces. It also observed three suspected but unconfirmed moons in the F Ring.[23] 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.[24] In 2007 Anthe was announced.[25] 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.[26] In March 2009, Aegaeon, a moonlet within the G Ring, was announced.[27] In July of the same year, S/2009 S 1, the first moonlet within the B Ring, was observed.[28] In April 2014, the possible beginning of a new moon, within the A Ring, was reported.[29] (related image)

Outer moons

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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 were discovered using ground-based telescopes.[30] 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.[31] They are probably fragments of larger bodies captured by Saturn's gravitational pull.[30][31] In 2005, astronomers using the Mauna Kea Observatory announced the discovery of twelve more small outer moons,[32][33] in 2006, astronomers using the Subaru 8.2 m telescope reported the discovery of nine more irregular moons,[34] 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.[35] 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.[13][3]

In 2019, researchers Edward Ashton, Brett Gladman, and Matthew Beaudoin conducted a survey of Saturn's Hill sphere using the 3.6-meter Canada–France–Hawaii Telescope and discovered about 80 new Saturnian irregular moons.[5][36] Follow-up observations of these new moons took place over 2019–2021, eventually leading to S/2019 S 1 being announced in November 2021 and an additional 62 moons being announced from 3–16 May 2023.[37][2] These discoveries brought Saturn's total number of confirmed moons up to 145, making it the first planet known to have over 100 moons.[37][38][39] Yet another moon, S/2006 S 20, was announced on 23 May 2023, bringing Saturn's total count moons to 146.[2] All of these new moons are small and faint, with diameters over 3 km (2 mi) and apparent magnitudes of 25–27.[5] The researchers found that the Saturnian irregular moon population is more abundant at smaller sizes, suggesting that they are 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 (1.7 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.[5]

Discovery of outer planet moons

  Moons of Jupiter
  Moons of Saturn
  Moons of Uranus
  Moons of Neptune

Naming

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Main article: Naming of moons

The modern names for Saturnian moons were suggested by John Herschel in 1847.[16] He proposed to name them after mythological figures associated with the Roman god of agriculture and harvest, Saturn (equated to the Greek Cronus).[16] In particular, the then known seven satellites were named after Titans, Titanesses and Giants – brothers and sisters of Cronus.[19] The idea was similar to Simon Marius' mythological naming scheme for the moons of Jupiter.[40]

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 Mimas] 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.[18][40] 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.[41] 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.[42]

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.

Physical characteristics

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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%.[b]

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 with the Moon
Name
 Diameter
(km)[43] 		Mass
(kg)[44] 		Orbital radius
(km)[45] 		Orbital period
(days)[45]
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

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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.[46] 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.[3] 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.[42]

Inner moons

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Ring moonlets

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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.[28] 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.[47]

In 2006, four tiny moonlets were found in Cassini images of the A Ring.[48] 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.[48] 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.[49] The moonlets themselves are tiny, ranging from about 40 to 500 meters in diameter, and are too small to be seen directly.[4]

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.[4] This region is relatively free from the disturbances caused by resonances with larger satellites,[4] 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.[49] 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.[4] 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.[29]

Similar moonlets may reside in the F Ring.[4] 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.[50]

One recently discovered moon, Aegaeon, resides within the bright arc of G Ring and is trapped in the 7:6 mean-motion resonance with Mimas.[27] 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.[51]

Ring shepherds

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Shepherd moon Daphnis in the Keeler gap
From top to bottom, 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), Prometheus (F Ring), Janus (A Ring), and Epimetheus (A Ring).[23][27] These moons 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.[46]

Janus and Epimetheus are co-orbital moons.[21] They are of similar size, with Janus being somewhat larger than Epimetheus.[46] They have orbits with less than a 100-kilometer 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.[52]

Other inner moons

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Other inner moons that are neither ring shepherds nor ring moonlets include Atlas and Pandora.

Inner large

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A circular part of a grayish surface, which is intersected from the top-left to the bottom-right by four wide sinuous groves. Smaller and shorter grooves can be seen between them running either parallel to the large grooves or criss-crossing them. There is a rough terrain in the top-left corner.
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.

  • Mimas is the smallest and least massive of the inner round moons,[44] although its mass is sufficient to alter the orbit of Methone.[52] 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.[53] Mimas has a large impact crater one-third its diameter, Herschel, situated on its leading hemisphere[54] Mimas has no known past or present geologic activity and its surface is dominated by impact craters, though it does have a water ocean 20-30 km beneath the surface.[55] The only tectonic features known are a few arcuate and linear troughs, which probably formed when Mimas was shattered by the Herschel impact.[54]
  • Enceladus is one of the smallest of Saturn's moons that is spherical in shape—only Mimas is smaller[53]—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.[56] 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.[56] 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.[56] These jets form a large plume off its south pole, which replenishes Saturn's E ring[56] and serves as the main source of ions in the magnetosphere of Saturn.[57] 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.[56] The source of the energy for this cryovolcanism is thought to be a 2:1 mean-motion resonance with Dione.[56] 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%.[56]
  • Tethys is the third largest of Saturn's inner moons.[44] 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.[54] 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.[54] 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.[54] 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.[43]
  • 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.[53] 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.[58] The troughs and lineaments are especially prominent on the trailing hemisphere, where several intersecting sets of fractures form what is called "wispy terrain".[58] The cratered plains have a few large impact craters reaching 250 km in diameter.[54] Smooth plains with low impact-crater counts are also present on a small fraction of its surface.[59] 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;[59] 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.[59]

Alkyonides

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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.[60] Of these three moons, only Methone has been photographed at close range, showing it to be egg-shaped with very few or no craters.[61]

Trojan

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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).[23] Helene is by far the largest trojan moon,[53] while Polydeuces is the smallest and has the most chaotic orbit.[52] These moons are coated with dusty material that has smoothed out their surfaces.[62]

Outer large

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Saturn's outer large 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:

  • Rhea is the second-largest of Saturn's moons. It is even slightly larger than Oberon, the second-largest moon of Uranus.[53] 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.[26] The depletion was hypothesized to be caused by the presence of dust-sized particles concentrated in a few faint equatorial rings.[26] Such a ring system would make Rhea the only moon in the Solar System known to have rings.[26] 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.[63] Otherwise Rhea has rather a typical heavily cratered surface,[54] with the exceptions of a few large Dione-type fractures (wispy terrain) on the trailing hemisphere[64] and a very faint "line" of material at the equator that may have been deposited by material deorbiting from present or former rings.[65] Rhea also has two very large impact basins on its anti-Saturnian hemisphere, which are about 400 and 500 km across.[64] The first, Tirawa, is roughly comparable to the Odysseus basin on Tethys.[54] There is also a 48 km-diameter impact crater called Inktomi[66][c] at 112°W that is prominent because of an extended system of bright rays,[67] which may be one of the youngest craters on the inner moons of Saturn.[64] No evidence of any endogenic activity has been discovered on the surface of Rhea.[64]
  • Titan, at 5,149 km diameter, is the second largest moon in the Solar System and Saturn's largest.[68][44] 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.[69] The dense atmosphere frequently produces bright white convective clouds, especially over the south pole region.[69] On 6 June 2013, scientists at the IAA-CSIC reported the detection of polycyclic aromatic hydrocarbons in the upper atmosphere of Titan.[70] 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.[71] 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.[69] It contains a pattern of light and dark regions, flow channels and possibly cryovolcanos.[69][72] Some dark regions are covered by longitudinal dune fields shaped by tidal winds, where sand is made of frozen water or hydrocarbons.[73] 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.[74] The largest lake, Kraken Mare, is larger than the Caspian Sea.[75] 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.[72] On 2 July 2014, NASA reported the ocean inside Titan may be "as salty as the Earth's Dead Sea".[76][77]
  • 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.[44] With an average diameter of about 270 km, Hyperion is smaller and lighter than Mimas.[78] 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.[78] The average density of about 0.55 g/cm3[78] 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.[78] It is the only moon besides the small moons of Pluto 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.[78] This makes the rotational behavior of Hyperion essentially unpredictable.[79]
  • Iapetus is the third-largest of Saturn's moons.[53] Orbiting the planet at 3.5 million km, it is by far the most distant of Saturn's large moons, and also has the largest orbital inclination, at 15.47°.[45] 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.[80] 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.[80] 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.[80] 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.[80] No evidence of any endogenic activity has been discovered.[80] 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.[81] 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.[81] 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.[82][83]

Irregular

[edit]
Diagram illustrating the orbits of the irregular satellites of Saturn (with Titan and Iapetus included for comparison). The inclination and semi-major axis are represented on the Y and X-axis, respectively. The satellites with inclinations below 90° are prograde, those above 90° are retrograde. The X-axis is labeled in terms of Saturn's Hill radius. The prograde Inuit and Gallic groups and the retrograde Norse group are identified.
Orbits and positions of Saturn's 122 irregular moons as of 25 February 2023. Prograde orbits are colored blue while retrograde orbits are colored red. Saturn's outermost regular moons, Titan, Hyperion, and Iapetus, are also shown with turquoise orbits.

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.[30] 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.[31] The irregulars generally have featureless visible and near infrared spectra dominated by water absorption bands.[30] They are neutral or moderately red in color—similar to C-type, P-type, or D-type asteroids,[42] though they are much less red than Kuiper belt objects.[30][d]

Inuit

[edit]
Main article: Inuit group

The Inuit group includes thirteen prograde outer moons that are similar enough in their distances from the planet (190–300 radii of Saturn), their orbital inclinations (45–50°) and their colors that they can be considered a group.[31][42] The Inuit group is further split into three distinct subgroups at different semi-major axes, and are named after their respective largest members. Ordered by increasing semi-major axis, these subgroups are the Kiviuq group, the Paaliaq group, and the Siarnaq group.[1] The Kiviuq group includes five members: Kiviuq, Ijiraq, S/2005 S 4, S/2019 S 1, and S/2020 S 1. The Siarnaq group includes seven members: Siarnaq, Tarqeq, S/2004 S 31, S/2019 S 14, S/2020 S 3, S/2019 S 6, and S/2020 S 5.[84] In contrast to the Kiviuq and Siarnaq subgroups, the Paaliaq subgroup does not contain any other known members besides Paaliaq itself.[1] Of the entire Inuit group, Siarnaq is the largest member with an estimated size of about 39 km.[85]

Gallic

[edit]
Main article: Gallic group

The Gallic group includes seven prograde outer moons that are similar enough in their distance from the planet (200–300 radii of Saturn), their orbital inclination (35–40°) and their color that they can be considered a group.[31][42] They are Albiorix, Bebhionn, Erriapus, Tarvos,[42] Saturn LX,[86] S/2007 S 8, and S/2020 S 4.[84] The largest of these moons is Albiorix with an estimated diameter of about 29 km.[85]

Norse

[edit]
Main article: Norse group

All 100 retrograde outer moons of Saturn are broadly classified into the Norse group.[31][42] 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,[42] and 69 unnamed satellites. After Phoebe, Ymir is the largest of the known retrograde irregular moons, with an estimated diameter of only 22 km.[1]

  • Phoebe, at 213±1.4 km in diameter, is by far the largest of Saturn's irregular satellites.[30] It has a retrograde orbit and rotates on its axis every 9.3 hours.[87] 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.[30] Cassini images revealed a dark surface scarred by numerous impacts—there are about 130 craters with diameters exceeding 10 km. Such impacts may have ejected fragments of Phoebe into orbit around Saturn—two of these may be S/2006 S 20 and S/2006 S 9, whose orbits are similar to Phoebe.[1][88][89] Spectroscopic measurement showed that the surface is made of water ice, carbon dioxide, phyllosilicates, organics and possibly iron-bearing minerals.[30] Phoebe is believed to be a captured centaur that originated in the Kuiper belt.[30] It also serves as a source of material for the largest known ring of Saturn, which darkens the leading hemisphere of Iapetus (see above).[81]

Outlier prograde satellites

[edit]

Two prograde moons of Saturn do not definitively belong to either the Inuit or Gallic groups.[1] S/2004 S 24 and S/2006 S 12 have similar orbital inclinations as the Gallic group, but have much more distant orbits with semi-major axes of ~400 Saturn radii and ~340 Saturn radii, respectively.[84][13][1]

List

[edit]
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

[edit]

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, green, 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, so the orbital elements of irregular moons listed here are averaged over a 5,000-year numerical integration by the Jet Propulsion Laboratory. These may sometimes strongly differ from the osculating orbital elements provided by other sources.[84][86] Their orbital elements are all based on a reference epoch of 1 January 2000.[84]

Key
  Small regular moons (17) ♠ Major moons (7) ♦ Inuit group (13)
♣ Gallic group (7) ‡ Norse group (100) § Outlier prograde irregular moons (2)
Label
[e] 		Name Pronunciation Image Abs.
magn.
[f] 		Diameter
(km)
[g] 		Mass
(×1015 kg)
[h] 		Semi-major
axis
(km)
[i] 		Orbital period (d)
[i][j] 		Inclination
(°)
[i][k] 		Eccentricity
[i] 		Position Discovery
year
[95] 		Year announced Discoverer
[41][95]
S/2009 S 1 —
— 0.3 ≈ 0.0000071  116900  0.47150 ≈ 0.0 ≈ 0.000 outer B Ring 2009 2009 Cassini[28]
(moonlets) —
A noisy image showing a few bright dots marked by circles
 — 0.04–0.4 < 0.000017 ≈ 130000 ≈ 0.55 ≈ 0.0 ≈ 0.000 Three 1,000 km bands within A Ring[4] 2006 — Cassini
XVIII Pan /ˈpæn/
An irregularly shaped body with a prominent equatorial ridge. It is illuminated from the bottom right.
 9.2 27.4
(34.6 × 28.2 × 21.0)		 4.30 133600 +0.57505 0.0 0.000 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.
 — 7.8
(9.8 × 8.4 × 5.6)		 0.068 136500 +0.59408 0.0 0.000 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.
 8.5 29.8
(40.8 × 35.4 × 18.6)		 5.490 137700 +0.60460 0.0 0.001 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.
 6.7 85.6
(137 × 81 × 56)		 159.72 139400 +0.61588 0.0 0.002 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.
 6.5 80.0
(103 × 79 × 63)		 135.7 141700 +0.63137 0.0 0.004 1980 1980 Voyager 1
XI Epimetheus /ɛpəˈmiːθiəs/
A partially-illuminated irregular body, which has a shape remotely resembling a cube. The body's surface consists of ridges and valleys and is covered by craters.
 5.5 117.2
(130 × 116 × 107)		 525.607 151400 +0.69701 0.3 0.020 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. 4.5 178.0
(203 × 186 × 149)		 1893.88 151500 +0.69735 0.2 0.007 co-orbital with Epimetheus 1966 1967 Dollfus
LIII Aegaeon /iːˈdʒiːɒn/
Image of Aegaeon by Cassini.
 — 0.66
(1.4 × 0.5 × 0.4)		 0.0000782 167500 +0.80812 0.0 0.000 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.
 3.2 396.4
(416 × 393 × 381)		 37509.4 186000 +0.94242 1.6 0.020   1789 1789 Herschel
XXXII Methone /məˈθoʊniː/
A smooth, featureless ellipsoidal object illuminated from the top right, distinctly looking like an egg.
 — 2.90
(3.88 × 2.58 × 2.42)		 0.00392 194700 +1.00955 0.0 0.002 Alkyonides 2004 2004 Cassini
XLIX Anthe /ˈænθiː/
A blurry ellipsoidal object in the center of the image
 — 1.8 ≈ 0.0015 198100 +1.03890 0.0 0.002 Alkyonides 2007 2007 Cassini
XXXIII Pallene /pəˈliːniː/
A small, half-illuminated ellipsoidal object in front of Saturn as a backdrop
 — 4.46
(5.76 × 4.16 × 3.68)		 ≈ 0.023 212300 +1.15606 0.2 0.004 Alkyonides 2004 2004 Cassini
II ♠Enceladus /ɛnˈsɛlədəs/
2.1 504.2
(513 × 503 × 497)		 108031.8 238400 +1.37022 0.0 0.005 Generates the E ring 1789 1789 Herschel
III ♠Tethys /ˈtiːθəs/
0.7 1062.2
(1077 × 1057 × 1053)		 617495.9 295000 +1.88780 1.1 0.001   1684 1684 Cassini
XIII Telesto /təˈlɛstoʊ/
An oblong object with a few large craters and a smooth surface
 8.7 24.6
(33.2 × 23.4 × 19.2)		 ≈ 3.9 295000 +1.88780 1.2 0.001 leading Tethys trojan (L4) 1980 1980 Smith et al.
XIV Calypso /kəˈlɪpsoʊ/
An oblong body is seen in this low resolution image.
 9.2 19.0
(29.4 × 18.6 × 12.8)		 ≈ 1.8 295000 +1.88780 1.5 0.001 trailing Tethys trojan (L5) 1980 1980 Pascu et al.
XII Helene /ˈhɛləniː/
An irregularly shaped body illuminated from the left. Its surface is covered by numerous impact craters.
 8.2 36.2
(45.2 × 39.2 × 26.6)		 7.1 377600 +2.73692 0.2 0.007 leading Dione trojan (L4) 1980 1980 Laques & Lecacheux
XXXIV Polydeuces /pɒliˈdjuːsiːz/
A small oblong body is barely resolved in this image.
 — 3.06
(3.50 × 3.10 × 2.62)		 ≈ 0.0075 377600 +2.73692 0.2 0.019 trailing Dione trojan (L5) 2004 2004 Cassini
IV ♠Dione /daɪˈoʊniː/
0.8 1122.8
(1128 × 1123 × 1119)		 1095486.8 377700 +2.73692 0.0 0.002   1684 1684 Cassini
V ♠Rhea /ˈreɪə/
0.1 1527.6
(1530 × 1526 × 1525)		 2306485.4 527200 +4.51750 0.3 0.001   1672 1673 Cassini
VI ♠Titan /ˈtaɪtən/
–1.3 5149.46
(5149 × 5149 × 5150)		 134518035.4 1221900 +15.9454 0.3 0.029   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)		 5551.0 1481500 +21.2767 0.6 0.105 in 4:3 resonance with Titan 1848 1848 Bond & Lassell
VIII ♠Iapetus /aɪˈæpətəs/
1.2 1468.6
(1491 × 1491 × 1424)		 1805659.1 3561700 +79.3310 7.6 0.028   1671 1673 Cassini
♦S/2019 S 1 —
15.3 ≈ 6 ≈ 0.11 11245400 +445.51 49.5 0.384 Inuit group (Kiviuq) 2019 2021 Ashton et al.
XXIV ♦Kiviuq /ˈkɪviək/
12.7 ≈ 19 ≈ 3.6 11307500 +449.13 48.0 0.275 Inuit group (Kiviuq) 2000 2000 Gladman et al.
♦S/2005 S 4 — 15.7 ≈ 5 ≈ 0.065 11324500 +450.22 48.0 0.315 Inuit group (Kiviuq) 2005 2023 Sheppard et al.
♦S/2020 S 1 — 15.9 ≈ 4 ≈ 0.034 11338600 +451.10 48.2 0.337 Inuit group (Kiviuq) 2020 2023 Ashton et al.
XXII ♦Ijiraq /ˈiːɪrɒk/
13.3 ≈ 15 ≈ 1.8 11344600 +451.43 49.2 0.293 Inuit group (Kiviuq) 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)		 8312.3 12929400 −550.30 175.2 0.164 Norse group (Phoebe) 1898 1899 Pickering
‡S/2006 S 20 — 15.7 ≈ 5 ≈ 0.065 13193700 −567.27 173.1 0.206 Norse group (Phoebe) 2006 2023 Sheppard et al.
‡S/2006 S 9 — 16.5 ≈ 3 ≈ 0.014 14406600 −647.89 173.0 0.248 Norse group (Phoebe) 2006 2023 Sheppard et al.
XX ♦Paaliaq /ˈpɑːliɒk/
11.7 ≈ 30 ≈ 14 14997900 +686.94 48.5 0.378 Inuit group (Paaliaq) 2000 2000 Gladman et al.
XXVII ‡Skathi /ˈskɑːði/
14.4 ≈ 9 ≈ 0.38 15575400 −728.09 151.6 0.281 Norse group 2000 2000 Gladman et al.
‡S/2007 S 5 — 16.2 ≈ 4 ≈ 0.034 15835700 −746.88 158.4 0.104 Norse group 2007 2023 Sheppard et al.
‡S/2007 S 7 — 16.2 ≈ 4 ≈ 0.034 15931600 −754.29 169.2 0.217 Norse group 2007 2023 Sheppard et al.
‡S/2007 S 2 — 15.6 ≈ 5 ≈ 0.065 15939100 −754.91 174.0 0.232 Norse group 2007 2007 Sheppard et al.
‡S/2004 S 37 — 15.9 ≈ 4 ≈ 0.034 15956500 −755.63 158.2 0.448 Norse group 2004 2019 Sheppard et al.
‡S/2004 S 47 — 16.3 ≈ 4 ≈ 0.034 16050700 −762.49 160.9 0.291 Norse group 2004 2023 Sheppard et al.
‡S/2004 S 40 — 16.3 ≈ 4 ≈ 0.034 16075600 −764.60 169.2 0.297 Norse group 2004 2023 Sheppard et al.
XXVI ♣Albiorix /ˌælbiˈɒrɪks/
11.2 28.6 ≈ 12 16329100 +783.46 36.8 0.482 Gallic group 2000 2000 Holman
‡S/2019 S 2 — 16.5 ≈ 3 ≈ 0.014 16560200 −799.85 173.3 0.279 Norse group 2019 2023 Ashton et al.
XXXVII ♣Bebhionn /ˈbeɪvɪn/
15.0 ≈ 7 ≈ 0.18 17027200 +834.85 38.5 0.459 Gallic group 2004 2005 Sheppard et al.
♣S/2007 S 8 — 16.0 ≈ 4 ≈ 0.034 17049000 +836.90 36.2 0.490 Gallic group 2007 2023 Sheppard et al.
LX ♣S/2004 S 29 — 15.8 ≈ 5 ≈ 0.065 17064100 +837.78 38.6 0.485 Gallic group 2004 2019 Sheppard et al.
‡S/2019 S 3 — 16.2 ≈ 4 ≈ 0.034 17077100 −837.74 166.9 0.249 Norse group 2019 2023 Ashton et al.
‡S/2020 S 7 — 16.8 ≈ 3 ≈ 0.014 17394000 −861.25 161.4 0.500 Norse group 2020 2023 Ashton et al.
♦S/2004 S 31 — 15.6 ≈ 5 ≈ 0.065 17497200 +866.09 48.1 0.159 Inuit group (Siarnaq) 2004 2019 Sheppard et al.
XXVIII ♣Erriapus /ɛriˈæpəs/
13.7 ≈ 12 ≈ 0.95 17507000 +871.09 37.1 0.476 Gallic group 2000 2000 Gladman et al.
XLVII ‡Skoll /ˈskɒl/
15.4 ≈ 6 ≈ 0.11 17623700 −878.38 159.4 0.463 Norse group 2006 2006 Sheppard et al.
LII ♦Tarqeq /ˈtɑːrkeɪk/
14.8 ≈ 7 ≈ 0.18 17751000 +884.99 48.7 0.143 Inuit group (Siarnaq) 2007 2007 Sheppard et al.
♦S/2019 S 14 — 16.3 ≈ 4 ≈ 0.034 17853200 +893.15 46.2 0.172 Inuit group (Siarnaq) 2019 2023 Ashton et al.
‡S/2020 S 2 — 16.9 ≈ 3 ≈ 0.014 17869000 −897.59 170.7 0.152 Norse group 2020 2023 Ashton et al.
XXIX ♦Siarnaq /ˈsiːɑːrnək/
10.6 39.3 ≈ 32 17881100 +895.58 47.8 0.309 Inuit group (Siarnaq) 2000 2000 Gladman et al.
‡S/2019 S 4 — 16.5 ≈ 3 ≈ 0.014 17951800 −903.89 170.1 0.408 Norse group 2019 2023 Ashton et al.
♦S/2020 S 3 — 16.4 ≈ 3 ≈ 0.014 18057200 +908.19 46.0 0.142 Inuit group (Siarnaq) 2020 2023 Ashton et al.
‡S/2004 S 41 — 16.3 ≈ 4 ≈ 0.034 18095000 −914.62 165.7 0.301 Norse group 2004 2023 Sheppard et al.
♦S/2019 S 6 — 16.1 ≈ 4 ≈ 0.034 18205500 +919.71 46.4 0.120 Inuit group (Siarnaq) 2019 2023 Ashton et al.
XXI ♣Tarvos /ˈtɑːrvəs/
13.1 ≈ 16 ≈ 2.1 18215600 +926.43 37.8 0.522 Gallic group 2000 2000 Gladman et al.
♣S/2020 S 4 — 17.0 ≈ 3 ≈ 0.014 18236000 +926.96 40.1 0.495 Gallic group 2020 2023 Ashton et al.
‡S/2004 S 42 — 16.1 ≈ 4 ≈ 0.034 18240800 −925.91 165.7 0.157 Norse group 2004 2023 Sheppard et al.
XLIV ‡Hyrrokkin /hɪˈrɒkən/
14.3 ≈ 9 ≈ 0.38 18341000 −931.90 149.9 0.336 Norse group 2004 2005 Sheppard et al.
LI ‡Greip /ˈɡreɪp/
15.3 ≈ 6 ≈ 0.11 18379800 −937.00 174.2 0.317 Norse group 2006 2006 Sheppard et al.
♦S/2020 S 5 — 16.6 ≈ 3 ≈ 0.014 18391400 +933.89 48.2 0.220 Inuit group (Siarnaq) 2020 2023 Ashton et al.
‡S/2004 S 13 — 16.3 ≈ 4 ≈ 0.034 18453300 −942.57 169.0 0.265 Norse group 2004 2005 Sheppard et al.
‡S/2007 S 6 — 16.4 ≈ 3 ≈ 0.014 18544900 −949.50 166.5 0.169 Norse group 2007 2023 Sheppard et al.
XXV ‡Mundilfari /mʊndəlˈværi/
14.6 ≈ 8 ≈ 0.27 18588100 −952.86 167.1 0.212 Norse group 2000 2000 Gladman et al.
‡S/2006 S 1 — 15.6 ≈ 5 ≈ 0.065 18746200 −964.24 156.0 0.105 Norse group 2006 2006 Sheppard et al.
‡S/2004 S 43 — 16.3 ≈ 4 ≈ 0.034 18935000 −980.08 171.1 0.432 Norse group 2004 2023 Sheppard et al.
‡S/2006 S 10 — 16.4 ≈ 3 ≈ 0.014 18979900 −983.14 161.6 0.151 Norse group 2006 2023 Sheppard et al.
‡S/2019 S 5 — 16.6 ≈ 3 ≈ 0.014 19090400 −991.44 158.8 0.216 Norse group 2019 2023 Ashton et al.
LIV ‡Gridr /ˈɡriːðər/ 15.8 ≈ 5 ≈ 0.065 19250900 −1004.75 163.9 0.187 Norse group 2004 2019 Sheppard et al.
XXXVIII ‡Bergelmir /bɛərˈjɛlmɪər/
15.2 ≈ 6 ≈ 0.11 19268400 −1005.53 158.8 0.145 Norse group 2004 2005 Sheppard et al.
L ‡Jarnsaxa /jɑːrnˈsæksə/ 15.6 ≈ 5 ≈ 0.065 19273200 −1006.46 163.0 0.218 Norse group 2006 2006 Sheppard et al.
XXXI ‡Narvi /ˈnɑːrvi/
14.5 ≈ 8 ≈ 0.27 19285600 −1003.95 142.2 0.441 Norse group 2003 2003 Sheppard et al.
XXIII ‡Suttungr /ˈsʊtʊŋɡər/
14.6 ≈ 8 ≈ 0.27 19392000 −1016.70 175.7 0.116 Norse group 2000 2000 Gladman et al.
‡S/2004 S 44 — 15.8 ≈ 5 ≈ 0.065 19515400 −1026.16 167.7 0.129 Norse group 2004 2023 Sheppard et al.
§S/2006 S 12 — 16.2 ≈ 4 ≈ 0.034 19569800 +1035.06 38.6 0.542 Gallic group?[l] 2006 2023 Sheppard et al.
‡S/2007 S 3 — 15.7 ≈ 5 ≈ 0.065 19614000 −1034.45 173.8 0.150 Norse group 2007 2007 Sheppard et al.
‡S/2004 S 45 — 16.0 ≈ 4 ≈ 0.034 19693600 −1038.70 154.0 0.551 Norse group 2004 2023 Sheppard et al.
XLIII ‡Hati /ˈhɑːti/
15.4 ≈ 6 ≈ 0.11 19695400 −1040.05 165.4 0.372 Norse group 2004 2005 Sheppard et al.
‡S/2004 S 17 — 16.0 ≈ 4 ≈ 0.034 19699300 −1040.86 167.9 0.162 Norse group 2004 2005 Sheppard et al.
‡S/2006 S 11 — 16.5 ≈ 3 ≈ 0.014 19711900 −1042.29 174.1 0.143 Norse group 2004 2023 Sheppard et al.
‡S/2004 S 12 — 15.9 ≈ 4 ≈ 0.034 19801200 −1048.57 164.7 0.337 Norse group 2004 2005 Sheppard et al.
LIX ‡Eggther /ˈɛɡθɛər/ 15.4 ≈ 6 ≈ 0.11 19843900 −1052.32 165.0 0.157 Norse group 2004 2019 Sheppard et al.
‡S/2006 S 13 — 16.1 ≈ 4 ≈ 0.034 19953800 −1060.63 162.0 0.313 Norse group 2006 2023 Sheppard et al.
‡S/2007 S 9 — 16.1 ≈ 4 ≈ 0.034 20174600 −1078.07 159.3 0.360 Norse group 2007 2023 Sheppard et al.
‡S/2019 S 7 — 16.3 ≈ 4 ≈ 0.034 20184900 −1080.58 174.2 0.232 Norse group 2019 2023 Ashton et al.
‡S/2019 S 8 — 16.3 ≈ 4 ≈ 0.034 20286700 −1088.87 172.8 0.311 Norse group 2019 2023 Ashton et al.
XL ‡Farbauti /fɑːrˈbaʊti/ 15.8 ≈ 5 ≈ 0.065 20290500 −1087.26 156.2 0.249 Norse group 2004 2005 Sheppard et al.
XXX ‡Thrymr /ˈθrɪmər/
14.3 ≈ 9 ≈ 0.38 20330900 −1092.17 175.0 0.467 Norse group 2000 2000 Gladman et al.
XXXIX ‡Bestla /ˈbɛstlə/
14.6 ≈ 8 ≈ 0.27 20338300 −1087.17 138.3 0.486 Norse group 2004 2005 Sheppard et al.
‡S/2019 S 9 — 16.3 ≈ 4 ≈ 0.034 20358800 −1093.09 159.5 0.433 Norse group 2019 2023 Ashton et al.
‡S/2004 S 46 — 16.4 ≈ 3 ≈ 0.014 20513100 −1107.59 177.2 0.249 Norse group 2004 2023 Sheppard et al.
LV ‡Angrboda /ˈɑːŋɡərboʊðə/ 16.2 ≈ 4 ≈ 0.034 20591200 −1114.06 177.7 0.216 Norse group 2004 2019 Sheppard et al.
‡S/2019 S 11 — 16.2 ≈ 4 ≈ 0.034 20663600 −1115.00 144.6 0.513 Norse group 2019 2023 Ashton et al.
XXXVI ‡Aegir /ˈaɪ.ɪər/ 15.5 ≈ 5 ≈ 0.065 20664700 −1119.34 166.1 0.255 Norse group 2004 2005 Sheppard et al.
‡S/2019 S 10 — 16.7 ≈ 3 ≈ 0.014 20700500 −1121.99 163.9 0.248 Norse group 2019 2023 Ashton et al.
LXI ‡Beli /ˈbiːli/ 16.1 ≈ 4 ≈ 0.034 20703800 −1121.74 158.9 0.087 Norse group 2004 2019 Sheppard et al.
‡S/2019 S 12 — 16.3 ≈ 4 ≈ 0.034 20894700 −1138.02 167.1 0.475 Norse group 2019 2023 Ashton et al.
LVII ‡Gerd /ˈjɛərð/ 15.9 ≈ 4 ≈ 0.034 20948500 −1142.97 174.4 0.518 Norse group 2004 2019 Sheppard et al.
‡S/2019 S 13 — 16.7 ≈ 3 ≈ 0.014 20964300 −1144.79 177.3 0.318 Norse group 2019 2023 Ashton et al.
‡S/2006 S 14 — 16.5 ≈ 3 ≈ 0.014 21062100 −1152.67 166.7 0.060 Norse group 2006 2023 Sheppard et al.
LXII ‡Gunnlod /ˈɡʊnlɒð/ 15.6 ≈ 5 ≈ 0.065 21141100 −1157.97 160.3 0.251 Norse group 2004 2019 Sheppard et al.
‡S/2019 S 15 — 16.6 ≈ 3 ≈ 0.014 21190300 −1161.60 157.8 0.257 Norse group 2019 2023 Ashton et al.
‡S/2020 S 6 — 16.6 ≈ 3 ≈ 0.014 21254200 −1167.94 166.9 0.480 Norse group 2020 2023 Ashton et al.
‡S/2004 S 7 — 15.6 ≈ 5 ≈ 0.065 21328200 −1173.93 164.9 0.511 Norse group 2004 2005 Sheppard et al.
‡S/2006 S 3 — 15.6 ≈ 5 ≈ 0.065 21353300 −1174.78 156.1 0.432 Norse group 2006 2006 Sheppard et al.
‡S/2005 S 5 — 16.4 ≈ 3 ≈ 0.014 21366100 −1177.82 169.5 0.588 Norse group 2005 2023 Sheppard et al.
LVI ‡Skrymir /ˈskrɪmɪər/ 15.6 ≈ 5 ≈ 0.065 21447600 −1185.10 175.6 0.437 Norse group 2004 2019 Sheppard et al.
‡S/2006 S 16 — 16.5 ≈ 3 ≈ 0.014 21720600 −1207.52 164.1 0.204 Norse group 2006 2023 Sheppard et al.
‡S/2006 S 15 — 16.2 ≈ 4 ≈ 0.034 21799400 −1213.96 161.1 0.117 Norse group 2006 2023 Sheppard et al.
‡S/2004 S 28 — 15.8 ≈ 5 ≈ 0.065 21865900 −1220.69 167.9 0.159 Norse group 2004 2019 Sheppard et al.
‡S/2020 S 8 — 16.4 ≈ 3 ≈ 0.014 21966600 −1228.11 161.8 0.252 Norse group 2020 2023 Ashton et al.
LXV ‡Alvaldi /ɔːlˈvɔːldi/ 15.6 ≈ 5 ≈ 0.065 21994200 −1232.18 177.4 0.238 Norse group 2004 2019 Sheppard et al.
XLV ‡Kari /ˈkɑːri/
14.5 ≈ 8 ≈ 0.27 22032800 −1231.19 153.0 0.469 Norse group 2006 2006 Sheppard et al.
‡S/2004 S 48 — 16.0 ≈ 4 ≈ 0.034 22136800 −1242.41 161.9 0.374 Norse group 2004 2023 Sheppard et al.
LXVI ‡Geirrod /ˈjeɪrɒd/ 15.9 ≈ 4 ≈ 0.034 22260000 −1251.15 154.3 0.539 Norse group 2004 2019 Sheppard et al.
XLI ‡Fenrir /ˈfɛnrɪər/ 15.9 ≈ 4 ≈ 0.034 22330000 −1260.19 164.5 0.137 Norse group 2004 2005 Sheppard et al.
‡S/2004 S 50 — 16.4 ≈ 3 ≈ 0.014 22346000 −1260.44 164.0 0.450 Norse group 2004 2023 Sheppard et al.
‡S/2006 S 17 — 16.0 ≈ 4 ≈ 0.034 22384100 −1264.51 168.7 0.425 Norse group 2006 2023 Sheppard et al.
‡S/2004 S 49 — 16.0 ≈ 4 ≈ 0.034 22399800 −1264.25 159.7 0.453 Norse group 2004 2023 Sheppard et al.
‡S/2019 S 17 — 15.9 ≈ 4 ≈ 0.034 22724000 −1291.39 155.5 0.546 Norse group 2019 2023 Ashton et al.
XLVIII ‡Surtur /ˈsɜːrtər/ 15.8 ≈ 5 ≈ 0.065 22745700 −1295.60 168.4 0.448 Norse group 2006 2006 Sheppard et al.
‡S/2006 S 18 — 16.1 ≈ 4 ≈ 0.034 22760700 −1298.40 169.5 0.131 Norse group 2006 2023 Sheppard et al.
XLVI ‡Loge /ˈlɔɪ.eɪ/
15.4 ≈ 6 ≈ 0.11 22919200 −1311.80 168.1 0.191 Norse group 2006 2006 Sheppard et al.
XIX ‡Ymir /ˈiːmɪər/
12.4 ≈ 22 ≈ 5.6 22954500 −1315.08 172.3 0.338 Norse group 2000 2000 Gladman et al.
‡S/2019 S 19 — 16.5 ≈ 3 ≈ 0.014 23044700 −1317.83 151.8 0.458 Norse group 2019 2023 Ashton et al.
‡S/2019 S 18 — 16.6 ≈ 3 ≈ 0.014 23140700 −1327.06 154.6 0.509 Norse group 2019 2023 Ashton et al.
‡S/2004 S 21 — 16.2 ≈ 4 ≈ 0.034 23159300 −1328.58 153.2 0.394 Norse group 2004 2019 Sheppard et al.
‡S/2004 S 39 — 16.1 ≈ 4 ≈ 0.034 23192200 −1335.88 165.9 0.101 Norse group 2004 2019 Sheppard et al.
‡S/2019 S 16 — 16.7 ≈ 3 ≈ 0.014 23264100 −1340.93 162.0 0.250 Norse group 2019 2023 Ashton et al.
‡S/2004 S 53 — 16.2 ≈ 4 ≈ 0.034 23279800 −1342.44 162.6 0.240 Norse group 2004 2023 Sheppard et al.
§S/2004 S 24 — 16.0 ≈ 4 ≈ 0.034 23339000 +1341.34 37.4 0.071 Gallic group?[l] 2004 2019 Sheppard et al.
‡S/2004 S 36 — 16.1 ≈ 4 ≈ 0.034 23390300 −1349.37 153.3 0.625 Norse group 2004 2019 Sheppard et al.
LXIII ‡Thiazzi /θiˈætsi/ 15.9 ≈ 4 ≈ 0.034 23579000 −1366.69 158.8 0.512 Norse group 2004 2019 Sheppard et al.
‡S/2019 S 20 — 16.7 ≈ 3 ≈ 0.014 23679600 −1375.53 156.1 0.354 Norse group 2019 2023 Ashton et al.
‡S/2006 S 19 — 16.1 ≈ 4 ≈ 0.034 23801100 −1389.33 175.5 0.467 Norse group 2006 2023 Sheppard et al.
LXIV ‡S/2004 S 34 — 16.2 ≈ 4 ≈ 0.034 24144900 −1420.80 168.3 0.280 Norse group 2004 2019 Sheppard et al.
XLII ‡Fornjot /ˈfɔːrnjɒt/
15.1 ≈ 6 ≈ 0.11 24936700 −1494.11 170.0 0.213 Norse group 2004 2005 Sheppard et al.
‡S/2004 S 51 — 16.1 ≈ 4 ≈ 0.034 25208000 −1519.41 171.2 0.201 Norse group 2004 2023 Sheppard et al.
‡S/2020 S 10 — 16.9 ≈ 3 ≈ 0.014 25314700 −1527.21 165.6 0.296 Norse group 2020 2023 Ashton et al.
‡S/2020 S 9 — 16.0 ≈ 4 ≈ 0.034 25408500 −1532.65 161.4 0.531 Norse group 2020 2023 Ashton et al.
LVIII ‡S/2004 S 26 — 15.7 ≈ 5 ≈ 0.065 26098700 −1603.99 173.0 0.147 Norse group 2004 2019 Sheppard et al.
‡S/2019 S 21 — 16.2 ≈ 4 ≈ 0.034 26439500 −1636.37 171.9 0.155 Norse group 2019 2023 Ashton et al.
‡S/2004 S 52 — 16.5 ≈ 3 ≈ 0.014 26446800 −1633.87 165.3 0.292 Norse group 2004 2023 Sheppard et al.

Unconfirmed

[edit]

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.[23]

Name Image Diameter (km) Semi-major
axis (km)[52] 		Orbital
period (d)[52] 		Position Discovery year Status
S/2004 S 3 and S 4[m] ≈ 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

Spurious

[edit]

Two moons were claimed to be discovered by different astronomers but never seen again. Both moons were said to orbit between Titan and Hyperion.[96]

Hypothetical

[edit]

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.[97][98]

Temporary

[edit]

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.[99]

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

Formation

[edit]

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,[100] or that two large moons fused to form Titan, with the collision scattering icy debris that formed the mid-sized moons.[101] 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.[71] 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.[102]

See also

[edit]

Notes

[edit]
  1. ^ 62 moons were announced 3–16 May, 2023: S/2020 S 1, S/2006 S 9, S/2007 S 5, S/2004 S 40, S/2019 S 2, S/2019 S 3, S/2020 S 2, S/2020 S 3, S/2019 S 4, S/2004 S 41, S/2020 S 4, S/2020 S 5, S/2007 S 6, S/2004 S 42, S/2006 S 10, S/2019 S 5, S/2004 S 43, S/2004 S 44, S/2004 S 45, S/2006 S 11, S/2006 S 12, S/2019 S 6, S/2006 S 13, S/2019 S 7, S/2019 S 8, S/2019 S 9, S/2004 S 46, S/2019 S 10, S/2004 S 47, S/2019 S 11, S/2006 S 14, S/2019 S 12, S/2020 S 6, S/2019 S 13, S/2005 S 4, S/2007 S 7, S/2007 S 8, S/2020 S 7, S/2019 S 14, S/2019 S 15, S/2005 S 5, S/2006 S 15, S/2006 S 16, S/2006 S 17, S/2004 S 48, S/2020 S 8, S/2004 S 49, S/2004 S 50, S/2006 S 18, S/2019 S 16, S/2019 S 17, S/2019 S 18, S/2019 S 19, S/2019 S 20, S/2006 S 19, S/2004 S 51, S/2020 S 9, S/2004 S 52, S/2007 S 9, S/2004 S 53, S/2020 S 10, and S/2019 S 21 which were published in MPECs 2023-J21 to 2023-K05. One more moon, S/2006 S 20, was announced on 23 May 2023, which brings the final count to 146.[2][1]
  2. ^ The mass of the rings is about the mass of Mimas,[11] 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.
  3. ^ Inktomi was once known as "The Splat".[67]
  4. ^ The photometric color may be used as a proxy for the chemical composition of satellites' surfaces.
  5. ^ A confirmed moon is given a permanent designation by the IAU consisting of a name and a Roman numeral.[41] 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.
  6. ^ Absolute magnitudes of regular satellites are calculated from their mean diameters and geometric albedos given in NASA's Saturnian Satellite Fact Sheet.[45] Absolute magnitude estimates for some small inner moons are not available as they do not have measured geometric albedos. Absolute magnitudes of irregular satellites were taken from the Minor Planet Center's Natural Satellites Ephemeris Service.[90] Calculations were made with NASA/JPL's Asteroid Size Estimator.[91]
  7. ^ The diameters and dimensions of the small inner moons, from Pan to Helene, are taken from Thomas et al., 2020, Table 1.[92] Diameters and dimensions of Mimas, Enceladus, Tethys, Dione, Rhea, Iapetus, and Phoebe are from Thomas 2010, Table 1.[43] Diameters of Siarnaq and Albiorix are from Grav et al., 2015, Table 3.[85] The approximate sizes of all other irregular satellites are calculated from their absolute magnitudes with an assumed geometric albedo of 0.04,[91] which is the average value for that population.[85]
  8. ^ Masses of the large round moons, including Hyperion, Phoebe, and Helene, were taken from Jacobson et al., 2022, Table 5.[93] Masses of Atlas, Prometheus, Pandora, Epimetheus, and Janus were taken from Lainey et al., 2023, Table 1.[94] Masses of Pan, Daphnis, Aegaeon, Methone, and Pallene were taken from Thomas et al., 2020, Table 2.[92] Masses of other regular satellites were calculated by multiplying their volumes with an assumed density of 500 kg/m3 (0.5 g/cm3), while masses of irregular satellites were calculated with an assumed density of 1000 kg/m3 (1.0 g/cm3).
  9. ^ a b c d Time-averaged orbital elements of all satellites were taken from JPL Solar System Dynamics.[84]
  10. ^ Negative orbital periods indicate a retrograde orbit around Saturn (opposite to the planet's rotation). Orbital periods of irregular satellites may not directly correlate with their semi-major axes due to perturbations.
  11. ^ Orbital inclinations of regular satellites and Phoebe are with respect to the Laplace plane. Orbital inclinations of irregular satellites are with respect to the ecliptic.[84]
  12. ^ a b May be part of the Gallic group because it has a similar inclination; however, it has a more distant semi-major axis.[1]
  13. ^ S/2004 S 4 was most likely a transient clump—it has not been recovered since the first sighting.[23]

References

[edit]
  1. ^ a b c d e f g h i Sheppard, Scott S.; Gladman, Brett J.; Alexandersen, Mike A.; Trujillo, Chadwick A. (May 2023). "New Jupiter and Saturn Satellites Reveal New Moon Dynamical Families". Research Notes of the American Astronomical Society. 7 (5): 100. Bibcode:2023RNAAS...7..100S. doi:10.3847/2515-5172/acd766. 100.
  2. ^ a b c "MPEC 2023-K118 : S/2006 S 20". Minor Planet Electronic Circulars. Minor Planet Center. 23 May 2023. Archived from the original on 25 May 2023. Retrieved 23 May 2023.
  3. ^ a b c Sheppard, Scott S. "Moons of Saturn". Earth & Planets Laboratory. Carnegie Institution for Science. Archived from the original on 7 October 2019. Retrieved 21 August 2022.
  4. ^ a b c d e f g h Tiscareno, Matthew S.; Burns, J.A; Hedman, M.M; Porco, C.C (2008). "The population of propellers in Saturn's A Ring". Astronomical Journal. 135 (3): 1083–1091. arXiv:0710.4547. Bibcode:2008AJ....135.1083T. doi:10.1088/0004-6256/135/3/1083. S2CID 28620198.
  5. ^ a b c d Ashton, Edward; Gladman, Brett; Beaudoin, Matthew (August 2021). "Evidence for a Recent Collision in Saturn's Irregular Moon Population". The Planetary Science Journal. 2 (4): 12. Bibcode:2021PSJ.....2..158A. doi:10.3847/PSJ/ac0979. S2CID 236974160.
  6. ^ Redd, Nola Taylor (27 March 2018). "Titan: Facts About Saturn's Largest Moon". Space.com. Archived from the original on 15 October 2017. Retrieved 7 October 2019.
  7. ^ "Enceladus - Overview - Planets - NASA Solar System Exploration". Archived from the original on 2013-02-17.
  8. ^ "Moons". Archived from the original on 2013-04-20. Retrieved 2013-02-13.
  9. ^ "Iapetus - NASA Science". science.nasa.gov. Archived from the original on 2024-01-06. Retrieved 2024-01-06.
  10. ^ "The View from Iapetus - NASA". Archived from the original on 2024-06-16. Retrieved 2024-01-06.
  11. ^ a b Esposito, L. W. (2002). "Planetary rings". Reports on Progress in Physics. 65 (12): 1741–1783. Bibcode:2002RPPh...65.1741E. doi:10.1088/0034-4885/65/12/201. S2CID 250909885.
  12. ^ "Help Name 20 Newly Discovered Moons of Saturn!". Carnegie Science. 7 October 2019. Archived from the original on 9 October 2019. Retrieved 9 October 2019.
  13. ^ a b c "Saturn Surpasses Jupiter After The Discovery Of 20 New Moons And You Can Help Name Them!". Carnegie Science. 7 October 2019. Archived from the original on 6 June 2020. Retrieved 7 October 2019.
  14. ^ Nemiroff, Robert & Bonnell, Jerry (March 25, 2005). "Huygens Discovers Luna Saturni". Astronomy Picture of the Day. Archived from the original on June 10, 2010. Retrieved March 4, 2010.
  15. ^ Baalke, Ron. "Historical Background of Saturn's Rings (1655)". NASA/JPL. Archived from the original on September 23, 2012. Retrieved March 4, 2010.
  16. ^ a b c d Van Helden, Albert (1994). "Naming the satellites of Jupiter and Saturn" (PDF). The Newsletter of the Historical Astronomy Division of the American Astronomical Society (32): 1–2. Archived from the original (PDF) on 2012-03-14.
  17. ^ Bond, W.C (1848). "Discovery of a new satellite of Saturn". Monthly Notices of the Royal Astronomical Society. 9: 1–2. Bibcode:1848MNRAS...9....1B. doi:10.1093/mnras/9.1.1. Archived from the original on 2020-11-21. Retrieved 2019-06-30.
  18. ^ a b Lassell, William (1848). "Discovery of new satellite of Saturn". Monthly Notices of the Royal Astronomical Society. 8 (9): 195–197. Bibcode:1848MNRAS...8..195L. doi:10.1093/mnras/8.9.195a. Archived from the original on 2020-11-21. Retrieved 2019-09-13.
  19. ^ a b Pickering, Edward C (1899). "A New Satellite of Saturn". Astrophysical Journal. 9 (221): 274–276. Bibcode:1899ApJ.....9..274P. doi:10.1086/140590. PMID 17844472.
  20. ^ a b Fountain, John W; Larson, Stephen M (1977). "A New Satellite of Saturn?". Science. 197 (4306): 915–917. Bibcode:1977Sci...197..915F. doi:10.1126/science.197.4306.915. PMID 17730174. S2CID 39202443.
  21. ^ a b c d e Uralskaya, V.S (1998). "Discovery of new satellites of Saturn". Astronomical and Astrophysical Transactions. 15 (1–4): 249–253. Bibcode:1998A&AT...15..249U. doi:10.1080/10556799808201777.
  22. ^ Corum, Jonathan (December 18, 2015). "Mapping Saturn's Moons". The New York Times. Archived from the original on May 20, 2020. Retrieved December 18, 2015.
  23. ^ a b c d e Porco, C. C.; Baker, E.; Barbara, J.; et al. (2005). "Cassini Imaging Science: Initial Results on Saturn's Rings and Small Satellites" (PDF). Science. 307 (5713): 1226–36. Bibcode:2005Sci...307.1226P. doi:10.1126/science.1108056. PMID 15731439. S2CID 1058405. Archived (PDF) from the original on 2011-07-25. Retrieved 2009-12-31.
  24. ^ Roy Britt, Robert (2004). "Hints of Unseen Moons in Saturn's Rings". Space.com. Archived from the original on February 12, 2006. Retrieved January 15, 2011.
  25. ^ Porco, C.; The Cassini Imaging Team (July 18, 2007). "S/2007 S4". IAU Circular. 8857. Archived from the original on March 27, 2012. Retrieved January 14, 2011.
  26. ^ a b c d Jones, G. H.; Roussos, E.; Krupp, N.; et al. (2008-03-07). "The Dust Halo of Saturn's Largest Icy Moon, Rhea". Science. 319 (5868): 1380–1384. Bibcode:2008Sci...319.1380J. doi:10.1126/science.1151524. ISSN 0036-8075. PMID 18323452. S2CID 206509814.
  27. ^ a b c Porco, C.; The Cassini Imaging Team (March 3, 2009). "S/2008 S1 (Aegaeon)". IAU Circular. 9023. Archived from the original on May 1, 2019. Retrieved March 4, 2009.
  28. ^ a b c Porco, C. & the Cassini Imaging Team (November 2, 2009). "S/2009 S1". IAU Circular. 9091. Archived from the original on June 11, 2011. Retrieved January 17, 2010.
  29. ^ a b Platt, Jane; Brown, Dwayne (14 April 2014). "NASA Cassini Images May Reveal Birth of a Saturn Moon". NASA. Archived from the original on 10 April 2019. Retrieved 14 April 2014.
  30. ^ a b c d e f g h i Jewitt, David; Haghighipour, Nader (September 2007). "Irregular Satellites of the Planets: Products of Capture in the Early Solar System" (PDF). Annual Review of Astronomy and Astrophysics. 45 (1): 261–295. arXiv:astro-ph/0703059. Bibcode:2007ARA&A..45..261J. doi:10.1146/annurev.astro.44.051905.092459. ISSN 0066-4146. S2CID 13282788. Archived from the original (PDF) on 2009-09-19.
  31. ^ a b c d e f Gladman, Brett; Kavelaars, J. J.; Holman, Matthew; Nicholson, Philip D.; Burns, Joseph A.; Hergenrother, Carl W.; Petit, Jean-Marc; Marsden, Brian G.; Jacobson, Robert; Gray, William; Grav, Tommy; et al. (July 2001). "Discovery of 12 satellites of Saturn exhibiting orbital clustering". Nature. 412 (6843): 163–166. Bibcode:2001Natur.412..163G. doi:10.1038/35084032. ISSN 0028-0836. PMID 11449267. S2CID 4420031.
  32. ^ Jewitt, David (May 3, 2005). "12 New Moons For Saturn". University of Hawaii. Archived from the original on July 16, 2011. Retrieved April 27, 2010.
  33. ^ Lakdawalla, Emily (May 3, 2005). "Twelve New Moons For Saturn". Archived from the original on May 14, 2008. Retrieved March 4, 2010.{{cite web}}: CS1 maint: bot: original URL status unknown (link)
  34. ^ Sheppard, S. S.; Jewitt, D. C. & Kleyna, J. (June 30, 2006). "Satellites of Saturn". IAU Circular. 8727. Archived from the original on February 13, 2010. Retrieved January 2, 2010.
  35. ^ Sheppard, S. S.; Jewitt, D. C. & Kleyna, J. (May 11, 2007). "S/2007 S 1, S/2007 S 2, and S/2007 S 3". IAU Circular. 8836: 1. Bibcode:2007IAUC.8836....1S. Archived from the original on February 13, 2010. Retrieved January 2, 2010.
  36. ^ Ashton, Edward; Gladman, Brett; Beaudoin, Matthew; Alexandersen, Mike; Petit, Jean-Marc (May 2022). "Discovery of the Closest Saturnian Irregular Moon, S/2019 S 1, and Implications for the Direct/Retrograde Satellite Ratio". The Astronomical Journal. 3 (5): 5. Bibcode:2022PSJ.....3..107A. doi:10.3847/PSJ/ac64a2. S2CID 248771843. 107.
  37. ^ a b "Saturn now leads moon race with 62 newly discovered moons". UBC Science. University of British Columbia. 11 May 2023. Archived from the original on 18 May 2023. Retrieved 11 May 2023.
  38. ^ O'Callaghan, Jonathan (12 May 2023). "With 62 Newly Discovered Moons, Saturn Knocks Jupiter Off Its Pedestal - If all the objects are recognized by scientific authorities, the ringed giant world will have 145 moons in its orbit". The New York Times. Archived from the original on 12 May 2023. Retrieved 13 May 2023.
  39. ^ Semeniuk, Ivan (14 May 2023). "Astronomers discover record-breaking 62 moons around Saturn". The Globe and Mail. Archived from the original on 30 January 2024. Retrieved 29 January 2024.
  40. ^ a b van Helden, Albert (August 1994). "Naming the Satellites of Jupiter and Saturn" (PDF). The Newsletter of the Historical Astronomy Division of the American Astronomical Society (32). Archived (PDF) from the original on 7 December 2022. Retrieved 10 March 2023.
  41. ^ a b c "Planet and Satellite Names and Discoverers". Gazetteer of Planetary Nomenclature. USGS Astrogeology. Archived from the original on 3 July 2010. Retrieved 22 January 2023.
  42. ^ a b c d e f g h Grav, T; Bauer, J (November 2007). "A deeper look at the colors of the saturnian irregular satellites". Icarus. 191 (1): 267–285. arXiv:astro-ph/0611590. Bibcode:2007Icar..191..267G. doi:10.1016/j.icarus.2007.04.020. S2CID 15710195.
  43. ^ a b c Thomas, P. C. (July 2010). "Sizes, shapes, and derived properties of the saturnian satellites after the Cassini nominal mission" (PDF). Icarus. 208 (1): 395–401. Bibcode:2010Icar..208..395T. doi:10.1016/j.icarus.2010.01.025. Archived from the original (PDF) on 2018-12-23. Retrieved 2015-09-04.
  44. ^ a b c d e Jacobson, R. A.; Antreasian, P. G.; Bordi, J. J.; Criddle, K. E.; Ionasescu, R.; Jones, J. B.; Mackenzie, R. A.; Meek, M. C.; Parcher, D.; Pelletier, F. J.; Owen, Jr., W. M.; Roth, D. C.; Roundhill, I. M.; Stauch, J. R. (December 2006). "The Gravity Field of the Saturnian System from Satellite Observations and Spacecraft Tracking Data". The Astronomical Journal. 132 (6): 2520–2526. Bibcode:2006AJ....132.2520J. doi:10.1086/508812.
  45. ^ a b c d Williams, David R. (August 21, 2008). "Saturnian Satellite Fact Sheet". NASA (National Space Science Data Center). Archived from the original on April 30, 2010. Retrieved April 27, 2010.
  46. ^ a b c Porco, C. C.; Thomas, P. C.; Weiss, J. W.; Richardson, D. C. (2007). "Saturn's Small Inner Satellites:Clues to Their Origins" (PDF). Science. 318 (5856): 1602–1607. Bibcode:2007Sci...318.1602P. doi:10.1126/science.1143977. PMID 18063794. S2CID 2253135. Archived (PDF) from the original on 2011-07-25. Retrieved 2015-08-28.
  47. ^ "A Small Find Near Equinox". NASA/JPL. August 7, 2009. Archived from the original on 2009-10-10. Retrieved January 2, 2010.
  48. ^ a b Tiscareno, Matthew S.; Burns, Joseph A; Hedman, Mathew M; Porco, Carolyn C.; Weiss, John W.; Dones, Luke; Richardson, Derek C.; Murray, Carl D. (2006). "100-metre-diameter moonlets in Saturn's A ring from observations of 'propeller' structures". Nature. 440 (7084): 648–650. Bibcode:2006Natur.440..648T. doi:10.1038/nature04581. PMID 16572165. S2CID 9688977.
  49. ^ a b Sremčević, Miodrag; Schmidt, Jürgen; Salo, Heikki; Seiß, Martin; Spahn, Frank; Albers, Nicole (2007). "A belt of moonlets in Saturn's A ring". Nature. 449 (7165): 1019–21. Bibcode:2007Natur.449.1019S. doi:10.1038/nature06224. PMID 17960236. S2CID 4330204.
  50. ^ Murray, Carl D.; Beurle, Kevin; Cooper, Nicholas J.; Evans, Michael W.; Williams, Gareth A.; Charnoz, Sébastien; et al. (June 2008). "The determination of the structure of Saturn's F ring by nearby moonlets" (PDF). Nature. 453 (7196): 739–744. Bibcode:2008Natur.453..739M. doi:10.1038/nature06999. ISSN 0028-0836. PMID 18528389. S2CID 205213483. Archived (PDF) from the original on 2020-03-05. Retrieved 2019-12-02.
  51. ^ Hedman, Matthew M.; Burns, Joseph A.; Tiscareno, Matthew S.; Porco, Carolyn C.; Jones, Geraint H.; Roussos, Elias; Krupp, Norbert; Paranicas, Chris; Kempf, Sascha (2007-08-03). "The Source of Saturn's G Ring" (PDF). Science. 317 (5838): 653–656. Bibcode:2007Sci...317..653H. doi:10.1126/science.1143964. ISSN 0036-8075. PMID 17673659. S2CID 137345. Archived (PDF) from the original on 2008-07-04.
  52. ^ a b c d e Spitale, J. N.; Jacobson, R. A.; Porco, C. C.; Owen, W. M. Jr. (2006). "The orbits of Saturn's small satellites derived from combined historic and Cassini imaging observations". The Astronomical Journal. 132 (2): 692–710. Bibcode:2006AJ....132..692S. doi:10.1086/505206. S2CID 26603974.
  53. ^ a b c d e f Thomas, P; Burns, J; Helfenstein, P; Squyres, S; Veverka, J; Porco, C; Turtle, E; Mcewen, A; Denk, T; Giese, B; et al. (October 2007). "Shapes of the saturnian icy satellites and their significance" (PDF). Icarus. 190 (2): 573–584. Bibcode:2007Icar..190..573T. doi:10.1016/j.icarus.2007.03.012. Archived (PDF) from the original on 2011-09-27.
  54. ^ a b c d e f g h Moore, Jeffrey M.; Schenk, Paul M.; Bruesch, Lindsey S.; Asphaug, Erik; McKinnon, William B. (October 2004). "Large impact features on middle-sized icy satellites" (PDF). Icarus. 171 (2): 421–443. Bibcode:2004Icar..171..421M. doi:10.1016/j.icarus.2004.05.009. Archived (PDF) from the original on 2018-10-02. Retrieved 2022-07-22.
  55. ^ Lainey, V; Rambaux, N; Tobie, G; Cooper, N; Zhang, Q; Noyelles, B; Baillié, K (2024-02-07). "A recently formed ocean inside Saturn's moon Mimas". Nature. 626 (7998): 280–282. Bibcode:2024Natur.626..280L. doi:10.1038/s41586-023-06975-9. ISSN 1476-4687. PMID 38326592. S2CID 267546453. Archived from the original on 2024-06-16. Retrieved 2024-02-07.
  56. ^ a b c d e f g Porco, C. C.; Helfenstein, P.; Thomas, P. C.; Ingersoll, A. P.; Wisdom, J.; West, R.; Neukum, G.; Denk, T.; Wagner, R. (10 March 2006). "Cassini Observes the Active South Pole of Enceladus". Science. 311 (5766): 1393–1401. Bibcode:2006Sci...311.1393P. doi:10.1126/science.1123013. PMID 16527964. S2CID 6976648. Archived from the original on 16 June 2024. Retrieved 16 February 2024.
  57. ^ Pontius, D. H.; Hill, T. W. (September 2006). "Enceladus: A significant plasma source for Saturn's magnetosphere". Journal of Geophysical Research: Space Physics. 111 (A9): A09214. Bibcode:2006JGRA..111.9214P. doi:10.1029/2006JA011674. ISSN 0148-0227.
  58. ^ a b Wagner, R. J.; Neukum, G.; Stephan, K.; Roatsch; Wolf; Porco (2009). "Stratigraphy of Tectonic Features on Saturn's Satellite Dione Derived from Cassini ISS Camera Data". Lunar and Planetary Science. XL: 2142. Bibcode:2009LPI....40.2142W.
  59. ^ a b c Schenk, P. M.; Moore, J. M. (2009). "Eruptive Volcanism on Saturn's Icy Moon Dione". Lunar and Planetary Science. XL: 2465. Bibcode:2009LPI....40.2465S.
  60. ^ "Cassini Images Ring Arcs Among Saturn's Moons (Cassini Press Release)". Ciclops.org. September 5, 2008. Archived from the original on January 2, 2010. Retrieved January 1, 2010.
  61. ^ Lakdawalla, Emily. "Methone, an egg in Saturn orbit?". Planetary Society. Archived from the original on 27 April 2019. Retrieved 27 April 2019.
  62. ^ "Cassini goodies: Telesto, Janus, Prometheus, Pandora, F ring". The Planetary Society.
  63. ^ Tiscareno, Matthew S.; Burns, Joseph A.; Cuzzi, Jeffrey N.; Hedman, Matthew M. (July 2010). "Cassini imaging search rules out rings around Rhea". Geophysical Research Letters. 37 (14): L14205. arXiv:1008.1764. Bibcode:2010GeoRL..3714205T. doi:10.1029/2010GL043663. ISSN 0094-8276. S2CID 59458559.
  64. ^ a b c d Wagner, R. J.; Neukum, G.; Giese, B.; Roatsch; Denk; Wolf; Porco (2008). "Geology of Saturn's Satellite Rhea on the Basis of the High-Resolution Images from the Targeted Flyby 049 on Aug. 30, 2007". Lunar and Planetary Science. XXXIX (1391): 1930. Bibcode:2008LPI....39.1930W.
  65. ^ Schenk, Paul M.; McKinnon, W. B. (2009). "Global Color Variations on Saturn's Icy Satellites, and New Evidence for Rhea's Ring". American Astronomical Society. 41: 3.03. Bibcode:2009DPS....41.0303S.
  66. ^ "Rhea:Inktomi". USGS—Gazetteer of Planetary Nomenclature. Archived from the original on June 29, 2011. Retrieved April 28, 2010.
  67. ^ a b "Rhea's Bright Splat". CICLOPS. June 5, 2005. Archived from the original on October 6, 2012. Retrieved April 28, 2010.
  68. ^ Zebker1, Howard A.; Stiles, Bryan; Hensley, Scott; Lorenz, Ralph; Kirk, Randolph L.; Lunine, Jonathan I. (15 May 2009). "Size and Shape of Saturn's Moon Titan". Science. 324 (5929): 921–923. Bibcode:2009Sci...324..921Z. doi:10.1126/science.1168905. PMID 19342551. S2CID 23911201.{{cite journal}}: CS1 maint: numeric names: authors list (link)
  69. ^ a b c d Porco, Carolyn C.; Baker, Emily; Barbara, John; et al. (March 2005). "Imaging of Titan from the Cassini spacecraft" (PDF). Nature. 434 (7030): 159–168. Bibcode:2005Natur.434..159P. doi:10.1038/nature03436. ISSN 0028-0836. PMID 15758990. S2CID 4360680. Archived from the original (PDF) on 2011-07-25.
  70. ^ López-Puertas, Manuel (6 June 2013). "PAH's in Titan's Upper Atmosphere". CSIC. Archived from the original on 22 August 2016. Retrieved 6 June 2013.
  71. ^ a b Dyches, Preston; Clavin, Whitney (23 June 2014). "Titan's Building Blocks Might Pre-date Saturn" (Press release). Jet Propulsion Laboratory. Archived from the original on 9 September 2018. Retrieved 28 June 2014.
  72. ^ a b Lopes, R.M.C.; Mitchell, K.L.; Stofan, E.R.; et al. (February 2007). "Cryovolcanic features on Titan's surface as revealed by the Cassini Titan Radar Mapper" (PDF). Icarus. 186 (2): 395–412. Bibcode:2007Icar..186..395L. doi:10.1016/j.icarus.2006.09.006. Archived from the original (PDF) on 2019-12-06. Retrieved 2010-01-05.
  73. ^ Lorenz, R. D.; Wall, S.; Radebaugh, J.; et al. (May 2006). "The Sand Seas of Titan: Cassini RADAR Observations of Longitudinal Dunes" (PDF). Science. 312 (5774): 724–727. Bibcode:2006Sci...312..724L. doi:10.1126/science.1123257. ISSN 0036-8075. PMID 16675695. S2CID 39367926. Archived (PDF) from the original on 2018-07-23. Retrieved 2019-09-23.
  74. ^ Stofan, E. R.; Elachi, C.; Lunine, J. I.; et al. (January 2007). "The lakes of Titan" (PDF). Nature. 445 (7123): 61–64. Bibcode:2007Natur.445...61S. doi:10.1038/nature05438. ISSN 0028-0836. PMID 17203056. S2CID 4370622. Archived from the original (PDF) on 2018-10-06. Retrieved 2010-01-05.
  75. ^ "Titan:Kraken Mare". USGS—Gazetteer of Planetary Nomenclature. Archived from the original on June 5, 2011. Retrieved January 5, 2010.
  76. ^ Dyches, Preston; Brown, Dwayne (2 July 2014). "Ocean on Saturn Moon Could be as Salty as the Dead Sea". NASA. Archived from the original on 9 July 2014. Retrieved July 2, 2014.
  77. ^ Mitri, Giuseppe; Meriggiola, Rachele; Hayes, Alex; Lefevre, Axel; Tobie, Gabriel; Genova, Antonio; Lunine, Jonathan I.; Zebker, Howard (1 July 2014). "Shape, topography, gravity anomalies and tidal deformation of Titan". Icarus. 236: 169–177. Bibcode:2014Icar..236..169M. doi:10.1016/j.icarus.2014.03.018.
  78. ^ a b c d e Thomas, P. C.; Armstrong, J. W.; Asmar, S. W.; et al. (2007). "Hyperion's sponge-like appearance". Nature. 448 (7149): 50–53. Bibcode:2007Natur.448...50T. doi:10.1038/nature05779. PMID 17611535. S2CID 4415537.
  79. ^ Thomas, P.C.; Black, G.J.; Nicholson, P.D. (September 1995). "Hyperion: Rotation, Shape, and Geology from Voyager Images". Icarus. 117 (1): 128–148. Bibcode:1995Icar..117..128T. doi:10.1006/icar.1995.1147.
  80. ^ a b c d e Porco, C. C.; Baker, E.; Barbara, J.; et al. (2005-02-25). "Cassini Imaging Science: Initial Results on Phoebe and Iapetus" (PDF). Science. 307 (5713): 1237–1242. Bibcode:2005Sci...307.1237P. doi:10.1126/science.1107981. ISSN 0036-8075. PMID 15731440. S2CID 20749556. Archived (PDF) from the original on 2018-07-19. Retrieved 2019-06-30.
  81. ^ a b c Verbiscer, Anne J.; Skrutskie, Michael F.; Hamilton, Douglas P.; et al. (2009). "Saturn's largest ring". Nature. 461 (7267): 1098–1100. Bibcode:2009Natur.461.1098V. doi:10.1038/nature08515. PMID 19812546. S2CID 4349726.
  82. ^ Denk, T.; et al. (2009-12-10). "Iapetus: Unique Surface Properties and a Global Color Dichotomy from Cassini Imaging". Science. 327 (5964): 435–9. Bibcode:2010Sci...327..435D. doi:10.1126/science.1177088. PMID 20007863. S2CID 165865.
  83. ^ Spencer, J. R.; Denk, T. (2009-12-10). "Formation of Iapetus' Extreme Albedo Dichotomy by Exogenically Triggered Thermal Ice Migration". Science. 327 (5964): 432–5. Bibcode:2010Sci...327..432S. CiteSeerX 10.1.1.651.4218. doi:10.1126/science.1177132. PMID 20007862. S2CID 20663944.
  84. ^ a b c d e f g "Planetary Satellite Mean Elements". Jet Propulsion Laboratory. Archived from the original on 9 October 2024. Retrieved 9 October 2024.
  85. ^ a b c d Grav, T.; Bauer, J. M.; Mainzer, A. K.; Masiero, J. R.; Nugent, C. R.; Cutri, R. M.; et al. (August 2015). "NEOWISE: Observations of the Irregular Satellites of Jupiter and Saturn". The Astrophysical Journal. 809 (1): 9. arXiv:1505.07820. Bibcode:2015ApJ...809....3G. doi:10.1088/0004-637X/809/1/3. S2CID 5834661. 3.
  86. ^ a b Jacobson, Robert A.; Brozović, Marina; Mastrodemos, Nickolaos; Riedel, Joseph E.; Sheppard, Scott S. (December 2022). "Ephemerides of the Irregular Saturnian Satellites from Earth-based Astrometry and Cassini Imaging". The Astronomical Journal. 164 (6): 10. Bibcode:2022AJ....164..240J. doi:10.3847/1538-3881/ac98c7. 240.
  87. ^ Giese, Bernd; Neukum, Gerhard; Roatsch, Thomas; Denk, Tilmann; Porco, Carolyn C.; et al. (October 2006). "Topographic modeling of Phoebe using Cassini images" (PDF). Planetary and Space Science. 54 (12): 1156–1166. Bibcode:2006P&SS...54.1156G. doi:10.1016/j.pss.2006.05.027. Archived (PDF) from the original on 2011-07-25.
  88. ^ "S/2006 S 20 – Tilmann Denk". Archived from the original on 2024-06-16. Retrieved 2024-01-23.
  89. ^ "S/2006 S 9 – Tilmann Denk". Archived from the original on 2023-12-24. Retrieved 2024-01-23.
  90. ^ "Natural Satellites Ephemeris Service". Minor Planet Center. Archived from the original on 4 October 2022. Retrieved 22 January 2023. Selection of Objects → "All Saturnian outer irregular satellites" → Check "I require Orbital Elements" → Get Information
  91. ^ a b "Asteroid Size Estimator". Center for Near Earth Object Studies. NASA. Archived from the original on 21 February 2017. Retrieved 8 June 2023.
  92. ^ a b Thomas, P. C.; Helfenstein, P. (July 2020). "The small inner satellites of Saturn: Shapes, structures and some implications". Icarus. 344: 20. Bibcode:2020Icar..34413355T. doi:10.1016/j.icarus.2019.06.016. S2CID 197474587. 113355.
  93. ^ Jacobson, Robert A. (November 2022). "The Orbits of the Main Saturnian Satellites, the Saturnian System Gravity Field, and the Orientation of Saturn's Pole". The Astronomical Journal. 164 (5): 19. Bibcode:2022AJ....164..199J. doi:10.3847/1538-3881/ac90c9. 199.
  94. ^ Lainey, V.; Rambaux, N.; Cooper, N.; Dahoumane, R.; Zhang, Q. (February 2023). "Characterising the interior of five inner Saturnian moons using Cassini ISS data". Astronomy & Astrophysics. 670: 6. Bibcode:2023A&A...670L..25L. doi:10.1051/0004-6361/202244757. L25.
  95. ^ a b "Planetary Satellite Discovery Circumstances". Jet Propulsion Laboratory. 23 May 2023. Archived from the original on 27 September 2021. Retrieved 7 June 2023.
  96. ^ a b c Schlyter, Paul (2009). "Saturn's Ninth and Tenth Moons". Views of the Solar System (Calvin J. Hamilton). Archived from the original on May 22, 2010. Retrieved January 5, 2010.
  97. ^ "Saturn's rings could have come from a destroyed moon named Chrysalis". New Scientist. 15 September 2022. Archived from the original on 16 September 2022. Retrieved 16 September 2022.
  98. ^ Wisdom, Jack; Dbouk, Rola; Militzer, Burkhard; Hubbard, William B.; Nimmo, Francis; Downey, Brynna G.; French, Richard G. (September 16, 2022). "Loss of a satellite could explain Saturn's obliquity and young rings". Science. 377 (6612): 1285–1289. Bibcode:2022Sci...377.1285W. doi:10.1126/science.abn1234. hdl:1721.1/148216. PMID 36107998. S2CID 252310492.
  99. ^ Deen, Sam. "P/2020 F1 (Leonard): A previous-perihelion precovery, and a very, very young comet". groups.io. Archived from the original on 27 March 2020. Retrieved 27 March 2020.
  100. ^ Canup, R. (December 2010). "Origin of Saturn's rings and inner moons by mass removal from a lost Titan-sized satellite". Nature. 468 (7326): 943–6. Bibcode:2010Natur.468..943C. doi:10.1038/nature09661. PMID 21151108. S2CID 4326819.
  101. ^ Asphaug, Erik; Reufer, Andreas (March 2013). "Late origin of the Saturn system". Icarus. 223 (1): 544–565. Bibcode:2013Icar..223..544A. doi:10.1016/j.icarus.2012.12.009. Archived from the original on 2023-05-27.
  102. ^ SETI Institute (March 25, 2016). "Moons of Saturn may be younger than the dinosaurs". Astronomy. Archived from the original on December 6, 2019. Retrieved March 30, 2016.
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