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In October 2013, a scientist wrote three words down on a piece of paper. They were simple words. A five-year-old could say them.   [New Trading View Logo]( [New Trading View Logo]( A note from the Editor: New Trading View is dedicated to providing readers like you with unique opportunities. The message below from one of our business associates is one we believe you should take a serious look at. Dear Investor, In October 2013, a scientist wrote three words down on a piece of paper. They were simple words. A five-year-old could say them. But these words hold the key to a new breakthrough the Economist says would be "A boon to humanity." And CNBC says, "Would help tens of millions of people." He began to tell fellow scientists the three words. And his ideas for them. He soon recruited a team that's been called "the best scientists on earth." Then he started telling investors about them. In May 2015 Fidelity Biosciences cut him a check for $217 million, along with an investor group. In August 2016, he told Jeff Bezos the three the words. He walked out with a check for $130 million. It took just over a year - 390 days - for his company to hit a $1 billion valuation. That's faster than any company in history, including Facebook. All because of three words. Words that all happen to start with the letter "B." [Discover the 3 words behind "the biggest drug ever" ]( How is that possible? It's because the three words hold the key to a new treatment Jim Cramer says would be "the biggest drug ever." A treatment that experts predict could help as many as 50 million people...and save the United States $20 trillion in medical costs. Any company that harnesses this treatment will thrive. Which is why a Big Pharma giant bought 11.2% of this small firm's stock last year. If you follow the lead of Bezos, Fidelity and the Big Pharma giant, you can lock in your stake in this firm today... And watch three words potentially get you a return of 113,548%. You have every right to be skeptical... But when I show you the three words and what they mean... You'll understand why so many people are rushing to back this visionary entrepreneur... And why The Wall Street Journal says, "The financial benefits would be massive." These three words could do more than just make you rich. They can change how we treat one of the cruelest diseases on earth. [Discover the 3 words behind "the biggest drug ever" ]( "The Buck Stops Here" [Signature] Dylan Jovine CEO and Founder Behind the Markets   You are receiving our newsletter because you opted-in for it on one of our sister websites. Make sure you stay up to date with finance news by [whitelisting us](. Copyright © 2023 New Trading View.com All Rights Reserved[.]( This ad is sent on behalf of Behind The Markets, 4260 NW 1st Avenue, Suite # 55 Boca Raton, FL 33431 – 4264. If you would like to unsubscribe from receiving offers from Behind The Markets please [click here](. 234 5th Ave, New York, NY 10001, United States [Privacy Policy]( l [Terms & Conditions]( Thinking about unsubscribing? We hope not! But, if you must, the link is below. [Unsubscribe]( The rings of Saturn are the most extensive ring system of any planet in the Solar System. They consist of countless small particles, ranging in size from micrometers to meters,[1] that orbit around Saturn. The ring particles are made almost entirely of water ice, with a trace component of rocky material. There is still no consensus as to their mechanism of formation. Although theoretical models indicated that the rings were likely to have formed early in the Solar System's history,[2] newer data from Cassini suggested they formed relatively late.[3] Although reflection from the rings increases Saturn's brightness, they are not visible from Earth with unaided vision. In 1610, the year after Galileo Galilei turned a telescope to the sky, he became the first person to observe Saturn's rings, though he could not see them well enough to discern their true nature. In 1655, Christiaan Huygens was the first person to describe them as a disk surrounding Saturn.[4] The concept that Saturn's rings are made up of a series of tiny ringlets can be traced to Pierre-Simon Laplace,[4] although true gaps are few – it is more correct to think of the rings as an annular disk with concentric local maxima and minima in density and brightness.[2] On the scale of the clumps within the rings there is much empty space. The rings have numerous gaps where particle density drops sharply: two opened by known moons embedded within them, and many others at locations of known destabilizing orbital resonances with the moons of Saturn. Other gaps remain unexplained. Stabilizing resonances, on the other hand, are responsible for the longevity of several rings, such as the Titan Ringlet and the G Ring. Well beyond the main rings is the Phoebe ring, which is presumed to originate from Phoebe and thus to share its retrograde orbital motion. It is aligned with the plane of Saturn's orbit. Saturn has an axial tilt of 27 degrees, so this ring is tilted at an angle of 27 degrees to the more visible rings orbiting above Saturn's equator. Voyager 2 view of Saturn casting a shadow across its rings. Four satellites, two of their shadows and ring spokes are visible. History Early observations Detail of Galileo's drawing of Saturn in a letter to Belisario Vinta (1610) Galileo Galilei was the first to observe the rings of Saturn in 1610 using his telescope, but was unable to identify them as such. He wrote to the Duke of Tuscany that "The planet Saturn is not alone, but is composed of three, which almost touch one another and never move nor change with respect to one another. They are arranged in a line parallel to the zodiac, and the middle one (Saturn itself) is about three times the size of the lateral ones."[5] He also described the rings as Saturn's "ears". In 1612 the Earth passed through the plane of the rings and they became invisible. Mystified, Galileo remarked "I do not know what to say in a case so surprising, so unlooked for and so novel."[4] He mused, "Has Saturn swallowed his children?" — referring to the myth of the Titan Saturn devouring his offspring to forestall the prophecy of them overthrowing him.[5][6] He was further confused when the rings again became visible in 1613.[4] Early astronomers used anagrams as a form of commitment scheme to lay claim to new discoveries before their results were ready for publication. 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.[7][8][9] In 1657 Christopher Wren became Professor of Astronomy at Gresham College, London. He had been making observations of the planet Saturn from around 1652 with the aim of explaining its appearance. His hypothesis was written up in De corpore saturni, in which he came close to suggesting the planet had a ring. However, Wren was unsure whether the ring was independent of the planet, or physically attached to it. Before Wren's theory was published Christiaan Huygens presented his theory of the rings of Saturn. Immediately Wren recognised this as a better hypothesis than his own and De corpore saturni was never published. Robert Hooke was another early observer of the rings of Saturn, and noted the casting of shadows on the rings.[10] Huygens' ring theory and later developments Huygens' ring theory in Systema Saturnium (1659) Huygens began grinding lenses with his brother Constantijn in 1655 and was able to observe Saturn with greater detail using a 43× power refracting telescope that he designed himself. He was the first to suggest that Saturn was surrounded by a ring detached from the planet, and famously published the anagram: "aaaaaaa­ccccc­deeeeeg­hiiiiiii­llllmm­nnnnnnnnn­oooopp­qrrs­tttttuuuuu".[11] Three years later, he revealed it to mean Annuto cingitur, tenui, plano, nusquam coherente, ad eclipticam inclinato ("[Saturn] is surrounded by a thin, flat, ring, nowhere touching, inclined to the ecliptic").[12][4][13] He published his ring theory 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.[14] In 1675, Giovanni Domenico Cassini determined that Saturn's ring was composed of multiple smaller rings with gaps between them;[15] the largest of these gaps was later named the Cassini Division. This division is a 4,800-km (3000 mile) wide region between the A ring and B Ring.[16] In 1787, Pierre-Simon Laplace proved that a uniform solid ring would be unstable and suggested that the rings were composed of a large number of solid ringlets.[17][4][18] In 1859, James Clerk Maxwell demonstrated that a nonuniform solid ring, solid ringlets or a continuous fluid ring would also not be stable, indicating that the ring must be composed of numerous small particles, all independently orbiting Saturn.[19][18] Later, Sofia Kovalevskaya also found that Saturn's rings cannot be liquid ring-shaped bodies.[20][21] Spectroscopic studies of the rings which were carried out independently in 1895 by James Keeler of the Allegheny Observatory and by Aristarkh Belopolsky of the Pulkovo Observatory showed that Maxwell's analysis was correct.[22][23] Four robotic spacecraft have observed Saturn's rings from the vicinity of the planet. Pioneer 11's closest approach to Saturn occurred in September 1979 at a distance of 20,900 km (13,000 miles).[24] Pioneer 11 was responsible for the discovery of the F ring.[24] Voyager 1's closest approach occurred in November 1980 at a distance of 64,200 km (40,000 miles).[25] A failed photopolarimeter prevented Voyager 1 from observing Saturn's rings at the planned resolution; nevertheless, images from the spacecraft provided unprecedented detail of the ring system and revealed the existence of the G ring.[26] Voyager 2's closest approach occurred in August 1981 at a distance of 41,000 km (25,000 miles).[25] Voyager 2's working photopolarimeter allowed it to observe the ring system at higher resolution than Voyager 1, and to thereby discover many previously unseen ringlets.[27] Cassini spacecraft entered into orbit around Saturn in July 2004.[28] Cassini's images of the rings are the most detailed to-date, and are responsible for the discovery of yet more ringlets.[29] The rings are named alphabetically in the order they were discovered[30] (A and B in 1675 by Giovanni Domenico Cassini, C in 1850 by William Cranch Bond and his son George Phillips Bond, D in 1933 by Nikolai P. Barabachov and B. Semejkin, E in 1967 by Walter A. Feibelman, F in 1979 by Pioneer 11, and G in 1980 by Voyager 1). The main rings are, working outward from the planet, C, B and A, with the Cassini Division, the largest gap, separating Rings B and A. Several fainter rings were discovered more recently. The D Ring is exceedingly faint and closest to the planet. The narrow F Ring is just outside the A Ring. Beyond that are two far fainter rings named G and E. The rings show a tremendous amount of structure on all scales, some related to perturbations by Saturn's moons, but much unexplained.[30] Simulated appearance of Saturn as seen from Earth over the course of one Saturn year Saturn's axial inclination 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.[31] Earth makes passes through the ring plane every 13 to 15 years, about every half Saturn year, and there are about equal chances of either a single or three crossings occurring in each such occasion. 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. Favorable ring plane crossing viewing opportunities (with Saturn not close to the Sun) only come during triple crossings.[32][33][34] Saturn's equinoxes, when the Sun passes through the ring plane, are not evenly spaced; on each orbit the Sun is south of the ring plane for 13.7 Earth years, then north of the plane for 15.7 years.[n 1] Dates for its northern hemisphere autumnal equinoxes include 19 November 1995 and 6 May 2025, with northern vernal equinoxes on 11 August 2009 and 23 January 2039.[36] During the period around an equinox the illumination of most of the rings is greatly reduced, making possible unique observations highlighting features that depart from the ring plane.[37] Physical characteristics 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 100 km; 60 miles across) as well as ice, these silicate bodies would have accreted more ice and been expelled from the rings, due to gravitational interactions with the rings and tidal interaction with Saturn, into progressively wider orbits. Within the Roche limit, bodies of rocky material are dense enough to accrete additional material, whereas less-dense bodies of ice are not. Once outside the rings, the newly formed moons could have continued to evolve through random mergers. This process may explain the variation in silicate content of Saturn's moons out to Rhea, as well as the trend towards less silicate content closer to Saturn. Rhea would then be the oldest of the moons formed from the primordial rings, with moons closer to Saturn being progressively younger.[63] The brightness and purity of the water ice in Saturn's rings have also been cited as evidence that the rings are much younger than Saturn,[54] as the infall of meteoric dust would have led to a darkening of the rings. However, new research indicates that the B Ring may be massive enough to have diluted infalling material and thus avoided substantial darkening over the age of the Solar System. Ring material may be recycled as clumps form within the rings and are then disrupted by impacts. This would explain the apparent youth of some of the material within the rings.[64] Evidence suggesting a recent origin of the C ring has been gathered by researchers analyzing data from the Cassini Titan Radar Mapper, which focused on analyzing the proportion of rocky silicates within this ring. If much of this material was contributed by a recently disrupted centaur or moon, the age of this ring could be on the order of 100 million years or less. On the other hand, if the material came primarily from micrometeoroid influx, the age would be closer to a billion years.[65] The Cassini UVIS team, led by Larry Esposito, used stellar occultation to discover 13 objects, ranging from 27 metres (89') to 10 km (6 miles) across, within the F ring. They are translucent, suggesting they are temporary aggregates of ice boulders a few meters across. Esposito believes this to be the basic structure of the Saturnian rings, particles clumping together, then being blasted apart.[66] Research based on rates of infall into Saturn favors a younger ring system age of hundreds of millions of years. Ring material is continually spiraling down into Saturn; the faster this infall, the shorter the lifetime of the ring system. One mechanism involves gravity pulling electrically charged water ice grains down from the rings along planetary magnetic field lines, a process termed 'ring rain'. This flow rate was inferred to be 432–2870 kg/s using ground-based Keck telescope observations; as a consequence of this process alone, the rings will be gone in ~292+818 −124 million years.[67] While traversing the gap between the rings and planet in September 2017, the Cassini spacecraft detected an equatorial flow of charge-neutral material from the rings to the planet of 4,800–44,000 kg/s.[68] Assuming this influx rate is stable, adding it to the continuous 'ring rain' process implies the rings may be gone in under 100 million years.[67][69] Subdivisions and structures within the rings The densest parts of the Saturnian ring system are the A and B Rings, which are separated by the Cassini Division (discovered in 1675 by Giovanni Domenico Cassini). Along with the C Ring, which was discovered in 1850 and is similar in character to the Cassini Division, these regions constitute the main rings. The main rings are denser and contain larger particles than the tenuous dusty rings. The latter include the D Ring, extending inward to Saturn's cloud tops, the G and E Rings and others beyond the main ring system. These diffuse rings are characterised as "dusty" because of the small size of their particles (often about a μm); their chemical composition is, like the main rings, almost entirely water ice. The narrow F Ring, just off the outer edge of the A Ring, is more difficult to categorize; parts of it are very dense, but it also contains a great deal of dust-size particles. Natural-color mosaic of Cassini narrow-angle camera images of the unilluminated side of Saturn's D, C, B, A and F rings (left to right) taken on May 9, 2007 (distances are to the planet's center). Physical parameters of the rings Notes: (1) Names as designated by the International Astronomical Union, unless otherwise noted. Broader separations between named rings are termed divisions, while narrower separations within named rings are called gaps. (2) Data mostly from the Gazetteer of Planetary Nomenclature, a NASA factsheet and several papers.[70][71][72] (3) distance is to centre of gaps, rings and ringlets that are narrower than 1,000 km (600 miles) (4) unofficial name D Ring A Cassini image of the faint D Ring, with the inner C Ring below The D Ring is the innermost ring, and is very faint. In 1980, Voyager 1 detected within this ring three ringlets designated D73, D72 and D68, with D68 being the discrete ringlet nearest to Saturn. Some 25 years later, Cassini images showed that D72 had become significantly broader and more diffuse, and had moved planetward by 200 km (100 miles).[74] Present in the D Ring is a finescale structure with waves 30 km (20 miles) apart. First seen in the gap between the C Ring and D73,[74] the structure was found during Saturn's 2009 equinox to extend a radial distance of 19,000 km (12,000 miles) from the D Ring to the inner edge of the B Ring.[75][76] The waves are interpreted as a spiral pattern of vertical corrugations of 2 to 20 m amplitude;[77] 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.[74][75][78] A similar spiral pattern in Jupiter's main ring has been attributed to a perturbation caused by impact of material from Comet Shoemaker-Levy 9 in 1994.[75][79][80] C Ring 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. The C Ring is a wide but faint ring located inward of the B Ring. It was discovered in 1850 by William and George Bond, though William R. Dawes and Johann Galle also saw it independently. William Lassell termed it the "Crepe Ring" because it seemed to be composed of darker material than the brighter A and B Rings.[81] Its vertical thickness is estimated at 5 metres (16'), its mass at around 1.1 × 1018 kg, and its optical depth varies from 0.05 to 0.12.[citation needed] That is, between 5 and 12 percent of light shining perpendicularly through the ring is blocked, so that when seen from above, the ring is close to transparent. The 30-km wavelength spiral corrugations first seen in the D Ring were observed during Saturn's equinox of 2009 to extend throughout the C Ring (see above). Colombo Gap and Titan Ringlet The Colombo Gap lies in the inner C Ring. Within the gap lies the bright but narrow Colombo Ringlet, centered at 77,883 km (48,394 miles) from Saturn's center, which is slightly elliptical rather than circular. This ringlet is also called the Titan Ringlet as it is governed by an orbital resonance with the moon Titan.[82] At this location within the rings, the length of a ring particle's apsidal precession is equal to the length of Titan's orbital motion, so that the outer end of this eccentric ringlet always points towards Titan.[82] Maxwell Gap and Ringlet The Maxwell Gap lies within the outer part of the C Ring. It also contains a dense non-circular ringlet, the Maxwell Ringlet. In many respects this ringlet is similar to the ε ring of Uranus. There are wave-like structures in the middle of both rings. While the wave in the ε ring is thought to be caused by Uranian moon Cordelia, no moon has been discovered in the Maxwell gap as of July 2008.[83] B Ring The B Ring is the largest, brightest, and most massive of the rings. Its thickness is estimated as 5 to 15 m and its optical depth varies from 0.4 to greater than 5,[84] meaning that >99% of the light passing through some parts of the B Ring is blocked. The B Ring contains a great deal of variation in its density and brightness, nearly all of it unexplained. These are concentric, appearing as narrow ringlets, though the B Ring does not contain any gaps.[citation needed] In places, the outer edge of the B Ring contains vertical structures deviating up to 2.5 km (1½ miles) from the main ring plane. A 2016 study of spiral density waves using stellar occultations indicated that the B Ring's surface density is in the range of 40 to 140 g/cm2, lower than previously believed, and that the ring's optical depth has little correlation with its mass density (a finding previously reported for the A and C rings).[84][85] The total mass of the B Ring was estimated to be somewhere in the range of 7 to 24×1018 kg. This compares to a mass for Mimas of 37.5×1018 kg.[84] High resolution (about 3 km per pixel) color view of the inner-central B Ring (98,600 to 105,500 km; 61,300 to 65,600 miles from Saturn's center). The structures shown (from 40 km; 25 miles wide ringlets at center to 300–500 km; 200 to 300 miles wide bands at right) remain sharply defined at scales below the resolution of the image. The B Ring's outer edge, viewed near equinox, where shadows are cast by vertical structures up to 2.5 km (1½ miles) high, probably created by unseen embedded moonlets. The Cassini Division is at top. Spokes 0:08 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 Until 1980, the structure of the rings of Saturn was explained as being caused exclusively by the action of gravitational forces. Then images from the Voyager spacecraft showed radial features in the B Ring, known as spokes,[86][87] which could not be explained in this manner, as their persistence and rotation around the rings was not consistent with gravitational orbital mechanics.[88] The spokes appear dark in backscattered light, and bright in forward-scattered light (see images in Gallery); the transition occurs at a phase angle near 60°. The leading theory 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. The precise mechanism generating the spokes is still unknown, although it has been suggested that the electrical disturbances might be caused by either lightning bolts in Saturn's atmosphere or micrometeoroid impacts on the rings.[88] The spokes were not observed again until some twenty-five years later, this time by the Cassini space probe. The spokes were not visible when Cassini arrived at Saturn in early 2004. Some scientists speculated that the spokes would not be visible again until 2007, based on models attempting to describe their formation. Nevertheless, the Cassini imaging team kept looking for spokes in images of the rings, and they were next seen in images taken on 5 September 2005.[89] The spokes appear to be a seasonal phenomenon, disappearing in the Saturnian midwinter and midsummer and reappearing as Saturn comes closer to equinox. 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.[90] Moonlet In 2009, during equinox, a moonlet embedded in the B ring was discovered from the shadow it cast. It is estimated to be 400 m (1,300 ft) in diameter.[91] The moonlet was given the provisional designation S/2009 S 1. Cassini Division 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 Cassini Division is a region 4,800 km (3,000 mi) in width between Saturn's A Ring and B Ring. It was discovered in 1675 by Giovanni Cassini at the Paris Observatory using a refracting telescope that had a 2.5-inch objective lens with a 20-foot-long focal length and a 90x magnification.[92][93] From Earth it appears as a thin black gap in the rings. However, Voyager discovered that the gap is itself populated by ring material bearing much similarity to the C Ring.[83] The division may appear bright in views of the unlit side of the rings, since the relatively low density of material allows more light to be transmitted through the thickness of the rings (see second image in gallery).[citation needed] The inner edge of the Cassini Division is governed by a strong orbital resonance. Ring particles at this location orbit twice for every orbit of the moon Mimas.[94] The resonance causes Mimas' pulls on these ring particles to accumulate, destabilizing their orbits and leading to a sharp cutoff in ring density. Many of the other gaps between ringlets within the Cassini Division, however, are unexplained.[95] Huygens Gap The Huygens Gap is located at the inner edge of the Cassini Division. It contains the dense, eccentric Huygens Ringlet in the middle. 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. There is an additional narrow ringlet just outside the Huygens Ringlet.[83] A Ring "A Ring" redirects here. For the letter, see Å. The central ringlet of the A Ring's Encke Gap coincides with Pan's orbit, implying its particles oscillate in horseshoe orbits. The A Ring is the outermost of the large, bright rings. Its inner boundary is the Cassini Division and its sharp outer boundary is close to the orbit of the small moon Atlas. The A Ring is interrupted at a location 22% of the ring width from its outer edge by the Encke Gap. A narrower gap 2% of the ring width from the outer edge is called the Keeler Gap. The thickness of the A Ring is estimated to be 10 to 30 m, its surface density from 35 to 40 g/cm2 and its total mass as 4 to 5×1018 kg[84] (just under the mass of Hyperion). Its optical depth varies from 0.4 to 0.9.[84] Similarly to the B Ring, the A Ring's outer edge is maintained by orbital resonances, albeit in this case a more complicated set. It is primarily acted on by the 7:6 resonance with Janus and Epimetheus, with other contributions from the 5:3 resonance with Mimas and various resonances with Prometheus and Pandora.[96][97] Other orbital resonances also excite many spiral density waves in the A Ring (and, to a lesser extent, other rings as well), which account for most of its structure. These waves are described by the same physics that describes the spiral arms of galaxies. Spiral bending waves, also present in the A Ring and also described by the same theory, are vertical corrugations in the ring rather than compression waves.[98] In April 2014, NASA scientists reported observing the possible formative stage of a new moon near the outer edge of the A Ring.[99][100] Encke Gap The Encke Gap is a 325-km (200 mile) wide gap within the A ring, centered at a distance of 133,590 km (83,000 miles) from Saturn's center.[101] It is caused by the presence of the small moon Pan,[102] which orbits within it. Images from the Cassini probe have shown that there are at least three thin, knotted ringlets within the gap.[83] Spiral density waves visible on both sides of it are induced by resonances with nearby moons exterior to the rings, while Pan induces an additional set of spiraling wakes (see image in gallery).[83] Johann Encke himself did not observe this gap; it was named in honour of his ring observations. The gap itself was discovered by James Edward Keeler in 1888.[81] The second major gap in the A ring, discovered by Voyager, was named the Keeler Gap in his honor.[103] The Encke Gap is a gap because it is entirely within the A Ring. There was some ambiguity between the terms gap and division until the IAU clarified the definitions in 2008; before that, the separation was sometimes called the "Encke Division".[104] Keeler Gap Waves in the Keeler gap edges induced by the orbital motion of Daphnis (see also a stretched closeup view in the gallery). Near Saturn's equinox, Daphnis and its waves cast shadows on the A Ring. The Keeler Gap is a 42-km (26 mile) wide gap in the A ring, approximately 250 km (150 miles) from the ring's outer edge. The small moon Daphnis, discovered 1 May 2005, orbits within it, keeping it clear.[105] The moon's passage induces waves in the edges of the gap (this is also influenced by its slight orbital eccentricity).[83] Because the orbit of Daphnis is slightly inclined to the ring plane, the waves have a component that is perpendicular to the ring plane, reaching a distance of 1500 m "above" the plane.[106][107] The Keeler gap was discovered by Voyager, and named in honor of the astronomer James Edward Keeler. Keeler had in turn discovered and named the Encke Gap in honor of Johann Encke.[81] Propeller moonlets Propeller moonlet Santos-Dumont from lit (top) and unlit sides of rings Location of the first four moonlets detected in the A ring. In 2006, four tiny "moonlets" were found in Cassini images of the A Ring.[108] The moonlets themselves are only about a hundred metres in diameter, too small to be seen directly; what Cassini sees are the "propeller"-shaped disturbances the moonlets create, which are several km (miles) across. It is estimated that the A Ring contains thousands of such objects. In 2007, the discovery of eight more moonlets revealed that they are largely confined to a 3,000 km (2000 mile) belt, about 130,000 km (80,000 miles) from Saturn's center,[109] and by 2008 over 150 propeller moonlets had been detected.[110] One that has been tracked for several years has been nicknamed Bleriot.[111] Roche Division The Roche Division (passing through image center) between the A Ring and the narrow F Ring. Atlas can be seen within it. The Encke and Keeler gaps are also visible. The separation between the A ring and the F Ring has been named the Roche Division in honor of the French physicist Édouard Roche.[112] The Roche Division should not be confused with the Roche limit which is the distance at which a large object is so close to a planet (such as Saturn) that the planet's tidal forces will pull it apart.[113] Lying at the outer edge of the main ring system, the Roche Division is in fact close to Saturn's Roche limit, which is why the rings have been unable to accrete into a moon.[114] Like the Cassini Division, the Roche Division is not empty but contains a sheet of material.[citation needed] The character of this material is similar to the tenuous and dusty D, E, and G Rings.[citation needed] Two locations in the Roche Division have a higher concentration of dust than the rest of the region. These were discovered by the Cassini probe imaging team and were given temporary designations: R/2004 S 1, which lies along the orbit of the moon Atlas; and R/2004 S 2, centered at 138,900 km (86,300 miles) from Saturn's center, inward of the orbit of Prometheus.[115][116] [New Trading View Logo](