Rings of Saturn

In September 2023, astronomers reported studies suggesting that the rings of Saturn may have resulted from the collision of two moons "a few hundred million years ago".

Galileo used the anagram "smaismrmil­mepoeta­leumibu­nenugt­tauiras" for Altissimum planetam tergeminum observavi ("I have observed the most distant planet to have a triple form") for discovering the rings of Saturn.

[12] Huygens began grinding lenses with his father Constantijn in 1655 and was able to observe Saturn with greater detail using a 43× power refracting telescope that he designed himself.

[13] Three years later, he revealed it to mean Annulo cingitur, tenui, plano, nusquam coherente, ad eclipticam inclinato ("[Saturn] is surrounded by a thin, flat, ring, nowhere touching [the body of the planet], inclined to the ecliptic").

[14][4][15] He published his ring hypothesis in Systema Saturnium (1659) which also included his discovery of Saturn's moon, Titan, as well as the first clear outline of the dimensions of the Solar System.

[32] In September 2023, astronomers reported studies suggesting that the rings of Saturn may have resulted from the collision of two moons "a few hundred million years ago".

[5][6] Saturn's axial tilt is 26.7°, meaning that widely varying views of the rings, of which the visible ones occupy its equatorial plane, are obtained from Earth at different times.

The most recent ring plane crossings were on 22 May 1995, 10 August 1995, 11 February 1996 and 4 September 2009; upcoming events will occur on 23 March 2025, 15 October 2038, 1 April 2039 and 9 July 2039.

With an estimated local thickness of as little as 10 meters (32' 10")[40] and as much as 1 km (1093 yards),[41] they are composed of 99.9% pure water ice with a smattering of impurities that may include tholins or silicates.

Some gaps are cleared out by the passage of tiny moonlets such as Pan,[48] many more of which may yet be discovered, and some ringlets seem to be maintained by the gravitational effects of small shepherd satellites (similar to Prometheus and Pandora's maintenance of the F ring).

A hypothesis originally proposed by Édouard Roche in the 19th century is that the rings were once a moon of Saturn (named Veritas, after a Roman goddess who hid in a well).

[citation needed] A more traditional version of the disrupted-moon hypothesis is that the rings are composed of debris from a moon 400 to 600 km (200 to 400 miles) in diameter, slightly larger than Mimas.

[63] A more recent variant of this type of hypothesis by R. M. Canup is that the rings could represent part of the remains of the icy mantle of a much larger, Titan-sized, differentiated moon that was stripped of its outer layer as it spiraled into the planet during the formative period when Saturn was still surrounded by a gaseous nebula.

[68] The Cassini UVIS team, led by Larry Esposito, used stellar occultation to discover 13 objects, ranging from 27 meters (89') to 10 km (6 miles) across, within the F ring.

One mechanism involves gravity pulling electrically charged water ice grains down from the rings along planetary magnetic field lines, a process termed 'ring rain'.

[88][89] The waves are interpreted as a spiral pattern of vertical corrugations of 2 to 20 m amplitude;[90] the fact that the period of the waves is decreasing over time (from 60 km; 40 miles in 1995 to 30 km; 20 miles by 2006) allows a deduction that the pattern may have originated in late 1983 with the impact of a cloud of debris (with a mass of ≈1012 kg) from a disrupted comet that tilted the rings out of the equatorial plane.

The leading hypothesis regarding the spokes' composition is that they consist of microscopic dust particles suspended away from the main ring by electrostatic repulsion, as they rotate almost synchronously with the magnetosphere of Saturn.

Suggestions that the spokes may be a seasonal effect, varying with Saturn's 29.7-year orbit, were supported by their gradual reappearance in the later years of the Cassini mission.

This ringlet exhibits irregular azimuthal variations of geometrical width and optical depth, which may be caused by the nearby 2:1 resonance with Mimas and the influence of the eccentric outer edge of the B-ring.

[133] In 2008, further dynamism was detected, suggesting that small unseen moons orbiting within the F Ring are continually passing through its narrow core because of perturbations from Prometheus.

"[139] A faint dust ring is present around the region occupied by the orbits of Janus and Epimetheus, as revealed by images taken in forward-scattered light by the Cassini spacecraft in 2006.

"[150] A reanalysis of Feibelman's original observations, conducted in anticipation of the coming Saturn flyby by Pioneer 11, once again called the evidence for this outer ring "shaky.

"[151] Even polarimetric observations by Pioneer 11 failed to conclusively identify E Ring during its 1979 flyby, though "its existence was inferred from [particle, radiation, and magnetic field measurements].

In 2005, the source of the E Ring's material was determined to be cryovolcanic plumes[154][155] emanating from the "tiger stripes" of the south polar region of the moon Enceladus.

[167][168][169] Saturn's second largest moon Rhea has been hypothesized to have a tenuous ring system of its own consisting of three narrow bands embedded in a disk of solid particles.

[170][171] These putative rings have not been imaged, but their existence has been inferred from Cassini observations in November 2005 of a depletion of energetic electrons in Saturn's magnetosphere near Rhea.

The Magnetospheric Imaging Instrument (MIMI) observed a gentle gradient punctuated by three sharp drops in plasma flow on each side of the moon in a nearly symmetric pattern.

This could be explained if they were absorbed by solid material in the form of an equatorial disk containing denser rings or arcs, with particles perhaps several decimeters to approximately a meter in diameter.

A more recent piece of evidence consistent with the presence of Rhean rings is a set of small ultraviolet-bright spots distributed in a line that extends three quarters of the way around the moon's circumference, within 2 degrees of the equator.

[172] However, targeted observations by Cassini of the putative ring plane from several angles have turned up nothing, suggesting that another explanation for these enigmatic features is needed.

The full set of rings, imaged on 19 July 2013 as Saturn eclipses the Sun from the vantage of the Cassini orbiter , 1.2 million kilometres ( 3 4 million miles) distant. Earth appears as a dot at 4 o'clock, between the G and E rings – with its brightness artificially exaggerated in this photograph.
Detail of Galileo's drawing of Saturn in a letter to Belisario Vinta (1610)
Huygens' ring hypothesis in Systema Saturnium (1659)
Simulated image using color to present radio-occultation -derived particle size data. The attenuation of 0.94-, 3.6-, and 13-cm signals sent by Cassini through the rings to Earth shows abundance of particles of sizes similar to or larger than those wavelengths. Purple (B, inner A Ring) means few particles are < 5 cm (all signals similarly attenuated). Green and blue (C, outer A Ring) mean particles < 5 cm and < 1 cm, respectively, are common. White areas (B Ring) are too dense to transmit adequate signal. Other evidence shows rings A to C have a broad range of particle sizes, up to m across.
Saturn and its A, B and C rings in visible and (inset) infrared light. In the false-color IR view, greater water ice content and larger grain size lead to blue-green color, while greater non-ice content and smaller grain size yield a reddish hue.
Cassini space probe view of the unilluminated side of Saturn's rings (October 10, 2013).
A 2007 artist's impression of the aggregates of icy particles that form the 'solid' portions of Saturn's rings. These elongated clumps are continually forming and dispersing. The largest particles are a few meters across.
A Cassini image of the faint D Ring, with the inner C Ring below
View of the outer C Ring; the Maxwell Gap with the Maxwell Ringlet on its right side are above and right of center. The Bond Gap is above a broad light band towards the upper right; the Dawes Gap is within a dark band just below the upper right corner.
Dark spokes mark the B ring's sunlit side in low phase angle Cassini images. This is a low-bitrate video. Lo-res version of this video
The Cassini Division imaged from the Cassini spacecraft. The Huygens Gap lies at its right border; the Laplace Gap is towards the center. A number of other, narrower gaps are also present. The moon in the background is Mimas .
The central ringlet of the A Ring's Encke Gap coincides with Pan 's orbit, implying its particles oscillate in horseshoe orbits .
Pan 's motion through the A ring 's Encke Gap induces edge waves and (non-self-propagating) spiraling wakes [ 116 ] ahead of and inward of it. The other more tightly wound bands are spiral density waves .
Close up view of waves in the Keeler gap edges induced by the orbital motion of Daphnis .
Location of the first four moonlets detected in the A ring.
The Roche Division (passing through image center) between the A Ring and the F Ring. Atlas , the Encke Gap, and the Keeler Gap are visible.
The small moons Pandora (left) and Prometheus (right) orbit on either side of the F ring. Prometheus acts as a ring shepherd and is followed by dark channels that it has carved into the inner strands of the ring.
The outer rings seen back-illuminated by the Sun
The Anthe Ring Arc – the bright spot is Anthe
View of the E right with Enceladus and its south polar jets.
The backlit E ring, with Enceladus silhouetted against it. The moon's south polar jets erupt brighty below it.
Comparison of Saturn's E Ring tendrils between Cassini photos and computer simulations.
E Ring tendrils from Enceladus geysers - comparison of images (a, c) with computer simulations.
The Phoebe ring's huge extent dwarfs the main rings. Inset: 24 μm Spitzer image of part of the ring