Keynote lectures/Saturn

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The gaseous-object Saturn with rings is seen in approximate natural color by the Hubble Space Telescope. Credit: Hubble Heritage Team (AURA/STScI/NASA/ESA).

Saturn is studied using gaseous-object astronomy.

"Saturday is the day of Saturn, and the color of Saturn, according to astronomers, is said to be black".[1]

Planets[edit | edit source]

Saturn is imaged by Cassini about an Earth day and a half after equinox. Credit: NASA/JPL/Space Science Institute.
These views demonstrate the 29 year period for oppositions of Saturn and the dramatic changes in the appearance of the rings. Credit: Tom Ruen.
This is a simulation of Saturn's orbit around the Sun. Credit: Lookang.
This is a snapshot of the planetary orbital poles. Credit: Urhixidur.

The picture dictionary display at the top of this section shows Saturn's approximate position in the Sol (or Sun) or the Solar System.

"The Saturn system experienced equinox, when the sun lies directly over a planet's equator and seasons change, in August 2009. (A full Saturn “year” is almost 30 Earth years.)"[2]

In the second image down on the right Saturn is about an Earth day and a half after equinox.

In antiquity the classical planets were the non-fixed objects visible in the sky, known to various ancient cultures. The classical planets were therefore the Sun and Moon and the five non-earth planets of our solar system closest to the sun (and closest to the Earth); all easily visible without a telescope. They are Mercury, Venus, Mars, Jupiter, and Saturn.

The third image down on the right shows how the position of the rings appears throughout an orbit of Saturn around the Sun.

A simulation of the revolution of Saturn around the Sun is in the diagram which is the fourth image down on the right.

An orbital pole is either end of an imaginary line running through the center of an orbit perpendicular to the orbital plane, projected onto the celestial sphere. It is similar in concept to a celestial pole but based on the planet's orbit instead of the planet's rotation.

The north orbital pole of a celestial body is defined by the right-hand rule: If you curve the fingers of your right hand along the direction of orbital motion, with your thumb extended parallel to the orbital axis, the direction your thumb points is defined to be north.

At right, fifth image down, is a snapshot of the planetary orbital poles.[3] The field of view is about 30°. The yellow dot in the centre is the Sun's North pole. Off to the side, the orange dot is Jupiter's orbital pole. Clustered around it are the other planets: Mercury in pale blue (closer to the Sun than to Jupiter), "Venus in green, [the] Earth in blue, Mars in red, Saturn in violet, Uranus in grey [partly underneath Earth] and Neptune in lavender. Dwarf planet Pluto is the dotless cross off in Cepheus.

Some statistics on the orbit of Saturn around the Sun include

  1. size (semi-major axis): 1,426,666,422 km (9.53667594 A.U.),
  2. perihelion: 1,349,823,615 km,
  3. aphelion: 1,503,509,229 km,
  4. eccentricity: 0.05386179,
  5. circumference: 8,957,504,604 km,
  6. average velocity: 34,701 km/h,
  7. sidereal period: 29.447498 Earth years, 10,755.70 Earth days,
  8. inclination: 2.49 degrees, and
  9. equatorial inclination: 26.7 degrees.[4]

Saturn systems[edit | edit source]

This is a 2 minute exposure of Saturn and its moons with a 12.5" telescope. Credit: Kevin Heider.
This is a stellarium generated image of Saturn and its major moons as seen on 19 March 2008. Credit: Collection Pictures.

In the first image down on the right, Saturn is apparent magnitude 0.8 in this image taken at 2010-03-04 11:45 UT. Saturn is overexposed to bring out fainter objects, including some members of the Saturn system.

Objects visible in this photo:

  • Two bright background stars to the upper left of Saturn,
  • Iapetus: 2 o'clock position (directly above NGC 4179 at 4 o'clock), labeled I,
  • Titan: bright-outer moon (magnitude 8) at 3 o'clock, labeled T,
  • Dione: 3 o'clock inner moon, labeled D,
  • NGC 4179: 4 o'clock,
  • Hyperion: faint-outer moon (magnitude 14) at 9 o'clock, labeled H,
  • Rhea: inner moon at 9 o'clock, labeled R.

The second image down on the right and shows a stellarium simulation of Saturn and its major moons as they appeared on March 19, 2008.

Daphnis[edit | edit source]

The camera was pointing toward Daphnis, and the image was taken using the CL1 and GRN filters. Credit: NASA/JPL-Caltech/Space Science Institute.
The wavemaker moon, Daphnis, is featured in this view, taken by NASA's Cassini spacecraft. Credit: NASA/JPL-Caltech/Space Science Institute.

The image on the right was taken on 2017-01-16 13:06 (UTC) and received on Earth 2017-01-18 00:41 (UTC). The camera was pointing toward Daphnis, and the image was taken using the clear (CL1) and green (GRN) filters.

"The wavemaker moon, Daphnis, is featured in this view [second down on the right], taken as NASA's Cassini spacecraft made one of its ring-grazing passes over the outer edges of Saturn's rings on Jan. 16, 2017. This is the closest view of the small moon obtained yet."[5]

"Daphnis (5 miles or 8 kilometers across) orbits within the 42-kilometer (26-mile) wide Keeler Gap. Cassini's viewing angle causes the gap to appear narrower than it actually is, due to foreshortening."[5]

"The little moon's gravity raises waves in the edges of the gap in both the horizontal and vertical directions. Cassini was able to observe the vertical structures in 2009, around the time of Saturn's equinox (see PIA11654)."[5]

"Like a couple of Saturn's other small ring moons, Atlas and Pan, Daphnis appears to have a narrow ridge around its equator and a fairly smooth mantle of material on its surface -- likely an accumulation of fine particles from the rings. A few craters are obvious at this resolution. An additional ridge can be seen further north that runs parallel to the equatorial band."[5]

"Fine details in the rings are also on display in this image. In particular, a grainy texture is seen in several wide lanes which hints at structures where particles are clumping together. In comparison to the otherwise sharp edges of the Keeler Gap, the wave peak in the gap edge at left has a softened appearance. This is possibly due to the movement of fine ring particles being spread out into the gap following Daphnis' last close approach to that edge on a previous orbit."[5]

"A faint, narrow tendril of ring material follows just behind Daphnis (to its left). This may have resulted from a moment when Daphnis drew a packet of material out of the ring, and now that packet is spreading itself out."[5]

"The image was taken in visible (green) light with the Cassini spacecraft narrow-angle camera. The view was acquired at a distance of approximately 17,000 miles (28,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft, or phase, angle of 71 degrees. Image scale is 551 feet (168 meters) per pixel."[5]

Hyperion[edit | edit source]

This false-color view of Saturn's moon Hyperion reveals crisp details across the strange, tumbling moon's surface. Credit: NASA/JPL-Caltech/Space Science Institute.
Unlike most of the dull grey moons in the Solar System, Hyperion's color is a rosy tan, as this view shows. Credit: NASA/JPL/Space Science Institute.

"Hyperion is the largest of Saturn's irregular, nonspherical moons. Hyperion's mean radius is 83.9 miles (135 km), but since Hyperion is rather potato-shaped, its shape can be described in terms of its diameter along its three axes: 255 x 163 x 137 miles (410 x 260 x 220 km, respectively). Considering its odd shape, Hyperion is probably a remnant of a larger moon that was destroyed by a major impact."[6]

"Hyperion's density is slightly more than half that of water. This could be due to water ice with gaps (porosity) of more than 40 percent. Also, lighter materials, such as frozen methane or carbon dioxide, could make up part of Hyperion. This is consistent with the concept of Hyperion accreting from a number of smaller ice and rock bodies, but not having enough gravity to compact them. Thus, Hyperion might be similar to a large rubble pile."[6]

"Hyperion rotates chaotically, tumbling unpredictably through space as it orbits Saturn. Hyperion orbits at a mean distance of 933,000 miles (1,500,000 km) from Saturn in an eccentric orbit. This contributes to variations in the spin or rotation of Hyperion. A stronger effect on Hyperion's rotation is that it is in resonance with Saturn's largest moon, Titan, which orbits at 759,200 miles (1,221,850 km). Thus, the two objects speed up and slow down as they pass each other in a complex set of variations. Because Hyperion is much smaller than Titan, its rotation and orbit are affected vastly more than the larger moon, and Titan apparently keeps the Hyperion orbit eccentric rather than growing more circular over time."[6]

"The great distance from Saturn and resonance with Titan has also kept Hyperion from becoming tidally locked facing Saturn. Hyperion rotates roughly every 13 days during its 21-day orbit."[6]

"The most noticeable close-up feature of Hyperion is its deeply cratered surface. Hyperion and its sister outer moons, Phoebe and Iapetus, all show extensive cratering because they are Saturn's most distant moons and have experienced very little tidal warming that might blur or erase earlier features. However, the Hyperion craters are particularly deep and do not have significant rays of ejecta (although there appears to have been slumping or landslides inside many of the bigger craters). The result is a curiously punched-in look, somewhat like the surface of a sponge or a wasp nest. Planetary geologists have theorized that Hyperion's high-porosity and low density would crater more by compression than excavation."[6]

"Many of the crater walls on Hyperion are bright, which suggests an abundance of water ice. The crater floors are mostly the areas of the lowest albedo (a measure of how reflective the surface is) and greatest red coloration. This may be because the average temperature of roughly -300 degrees Fahrenheit (-180 degrees Celsius) might be close enough to a temperature that would cause volatiles to sublimate, leaving the darker materials accumulated on the crater floors. This scenario fits with some of the newer crater floors being bright water ice."[6]

Iapetus[edit | edit source]

Cassini captures the first high-resolution glimpse of the bright trailing hemisphere of Saturn's moon Iapetus. Credit: NASA/JPL/Space Science Institute.
Saturn's two-faced moon tilts and rotates for Cassini in this mesmerizing movie sequence of images acquired during the spacecraft's close encounter with Iapetus on Nov. 12, 2005. Credit: NASA/JPL/Space Science Institute.
This Cassini spacecraft view shows how the bright and dark regions on Iapetus fit together like the seams of a baseball. Credit: NASA/JPL/Space Science Institute.

"This false-color mosaic shows the entire hemisphere of Iapetus (1,468 kilometers, or 912 miles across) visible from Cassini on the outbound leg of its encounter with the two-toned moon in Sept. 2007."[7]

"Iapetus's leading hemisphere has a reflectivity (or albedo) as dark as coal (albedo 0.03-0.05 with a slight reddish tinge) and its trailing hemisphere is much brighter at 0.5-0.6."[7]

"Saturn's third largest moon, Iapetus has a mean radius of 457 miles (736 km) and a density only 1.2 times that of liquid water. It has been suggested that Iapetus (like Rhea) is three quarters ice and one quarter rock."[7]

"Iapetus orbits at 2,213,000 miles (3,561,000 km) from Saturn. The great distance from Saturn's tidal forces and from most of the other moons and ring particles has probably allowed the Iapetus surface to be largely unaffected by any melting episodes that could have caused some smoothing or "resurfacing" as on some of the moons closer to Saturn."[7]

"Saturn has tidally locked Iapetus. The moon always presents the same face toward Saturn. With its distant, inclined orbit, Iapetus is the only large moon from which there is a nice view of the rings of Saturn."[7]

"As with some other Saturnian moons, Iapetus is in resonance with Saturn's largest moon, Titan, which orbits at 759,200 miles (1,221,850 km). That means that the two objects speed up and slow down as they pass each other in a complex set of variations. However, Iapetus has a diameter less than a third of Titan's diameter, so Titan's rotation and orbit are affected much less than those of Iapetus."[7]

"The second most notable feature of Iapetus is its "equatorial ridge," a chain of 6-mile (10-km) high mountains girdling the moon's equator. On the anti-Saturnian side of Iapetus, the ridge appears to break up and distinct, partially bright mountains are observed. The Voyager I and Voyager II encounters provided the first knowledge of these mountains, and they are informally referred to as the Voyager Mountains."[7]

Mimas[edit | edit source]

View was captured by NASA's Cassini spacecraft on its closest-ever flyby of Saturn's moon Mimas. Credit: NASA.
Image is of the trailing side of Mimas taken by the Cassini spacecraft Aug. 2, 2005 Credit: NASA.

"Less than 123 miles (198 km) in mean radius, crater-covered Mimas is the smallest and innermost of Saturn's major moons. It is not quite big enough to hold a round shape, so it is somewhat ovoid with dimensions of 129 x 122 x 119 (miles 207 x 197 x 191 km, respectively). Its low density suggests that it consists almost entirely of water ice, which is the only substance ever detected on Mimas."[8]

"At a mean distance just over 115,000 miles (186,000 km) from the massive planet, Mimas takes only 22 hours and 36 minutes to complete an orbit. Mimas is tidally locked: it keeps the same face toward Saturn as it flies around the planet, just as our Moon does with Earth."[8]

"Most of the Mimas surface is saturated with impact craters ranging in size up to greater than 25 miles (40 km) in diameter. However, the craters in the South Pole region of Mimas are generally 12.4 miles (20 km) in diameter or less. This suggests that some melting or other resurfacing processes occurred there later than on the rest of the moon. (Interestingly, the South Pole area of Enceladus appears to be the source of that moon's geysers.)"[8]

"Its most distinguishing feature is a giant impact crater -- named Herschel after the moon's discoverer -- which stretches a third of the way across the face of the moon [...] The Herschel Crater is 80 miles (130 km) across -- one third of the diameter of the moon itself -- with outer walls about 3 miles (5 km) high and a central peak 3.5 miles (6 km) high. The impact that blasted this crater out of Mimas probably came close to breaking the moon apart. Shock waves from the Herschel impact may have caused the fractures, also called chasmata, on the opposite side of Mimas."[8]

"That Mimas appears to be frozen solid is puzzling because Mimas is closer to Saturn and has a much more eccentric (elongated) orbit than Enceladus, which should mean that Mimas has more tidal heating than Enceladus. Yet Enceladus displays geysers of water, which implies internal heat, while Mimas has one of the most heavily cratered surfaces in the solar system, which suggests a frozen surface that has persisted for enough time to preserve all those craters. This paradox has prompted the "Mimas Test" by which any theory that claims to explain the partially thawed water of Enceladus must also explain the entirely frozen water of Mimas."[8]

"Mimas orbits Saturn exactly twice as often as the more distant moon, Tethys, a phenomenon known as "orbital resonance." Similar orbital resonances between Mimas and parts of Saturn's rings are thought to be responsible for the Huygens gap, which marks the boundary between the B Ring and the Cassini Division, and for several density waves within the A Ring. In addition, Mimas' slight inclination (1.574 degrees with respect to the ring plane) gives rise to several vertical bending waves within the A Ring."[8]

"Mimas is in resonance with two nearby moons, Dione and Enceladus. That is, these moons speed up slightly as they approach each other and slow down as they draw away, causing their orbits to vary slightly in a long series of complex changes, which help keep them locked in their positions."[8]

"Mimas strongly perturbs the tiny 2-mile (3-km) diameter moon Methone, the 3-mile (4-km) diameter moon Pallene, and the 1-mile (2-km) diameter moon Anthe, all of which orbit between Mimas and the next major moon going out from Saturn, Enceladus. The vastly more massive Mimas causes the Methone orbit to vary by as much as 12.4 miles (20 km). The perturbations are larger for tiny Anthe, and slightly smaller for Pallene."[8]

Phoebe[edit | edit source]

The saturnian moon Phoebe is photographed by Cassini. Credit: NASA.

"Phoebe is one of Saturn's most intriguing moons, orbiting at a distance of 8,049,668 miles (12,952,000 km) from the planet, almost four times the distance from Saturn than its nearest neighbor, the moon Iapetus. Phoebe and Iapetus are the only major moons in the Saturnian system that do not orbit closely to the plane of Saturn's equator."[9]

"Phoebe is roughly spherical and has a mean radius of about 66.2 miles (106.5 km), about one-sixteenth the radius of Earth's Moon. Phoebe rotates on its axis every nine hours, and it completes a full orbit around Saturn in about 18 Earth months. Its irregular, elliptical orbit is inclined about 175 degrees to Saturn's equator. Phoebe's orbit is also retrograde, which means it goes around Saturn in the opposite direction than most other moons -- as well as most objects in the solar system."[9]

"Unlike most major moons orbiting Saturn, Phoebe is very dark and reflects only 6 percent of the sunlight it receives. Its darkness and irregular, retrograde orbit suggest Phoebe is most likely a captured object. A captured object is a celestial body that is trapped by the gravitational pull of a much bigger body, generally a planet. Phoebe's darkness, in particular, suggests that the small moon comes from the outer solar system, an area where there is plenty of dark material."[9]

"Phoebe could be a captured Centaur. Centaurs are believed to be Kuiper Belt bodies that migrated into the inner solar system. Centaurs are found between the asteroid belt and the Kuiper Belt, and are considered a kind of intermediate type of small body, neither an asteroid nor a Kuiper Belt object. If Phoebe is indeed a captured Centaur, images and scientific data of Phoebe taken by the Cassini spacecraft will give scientists the first opportunity to study a Centaur."[9]

Rhea[edit | edit source]

This giant mosaic reveals Saturn's icy moon Rhea in her full, crater-scarred glory. Credit: NASA/JPL/Space Science Institute.
This perspective view shows one of a series of relatively blue patches that form a very narrow band only 10 kilometers wide that straddles Rhea's equator. Credit: Paul Schenk, NASA/JPL/Space Science Institute/Universities Space Research Association/Lunar & Planetary Institute.
A bright fresh looking impact crater (Inktomi) on the leading hemisphere of Rhea has a diameter of 48 km and an extensive ray system. Credit: NASA/JPL/Space Science Institute.

"Rhea is the second largest moon of Saturn, but with a mean radius of 475 miles (764 km) it is less than a third the radius of Saturn's largest moon, Titan. Rhea is a small, cold, airless body that is very similar to sister moons Dione and Tethys. As with the other two moons, Rhea is tidally locked in phase with its parent -- one side always faces toward Saturn - as it completes its 4.5-Earth-day orbit around the planet. Rhea's surface temperatures are also similar to Dione and Tethys, being roughly as warm as -281 degrees Fahrenheit (-174 degrees Celsius) in sunlit areas and ranging down to -364 degrees Fahrenheit (-220 degrees Celsius) in shaded areas. Also like Dione and Tethys, Rhea has a high reflectivity (or geometric albedo) suggesting a surface composition largely of water ice, which behaves like rock in Rhea's temperature range."[10]

"Rhea's density of 1.233 times that of liquid water suggests that Rhea is three quarters ice and one quarter rock. Cassini spacecraft measurements from a close encounter showed a moment of inertia about its axis (a measure of how difficult it is to change its rotation) of a higher value than what would be expected if Rhea has a rocky core. Thus, it is thought that Rhea is composed of a homogenous mixture of ice and rock -- a frozen dirty snowball."[10]

"Rhea, at a distance of 327,500 miles (527,000 km), is farther away from Saturn than Dione and Tethys, and because of this Rhea does not receive ample tidal variation from Saturn to cause internal heating. This has an important effect. Both Dione and Tethys have more areas of smooth plains than Rhea. Such plains are probably areas where liquid water reached the surface and ponded in depressions such as craters, forming flat surfaces before refreezing and thus erasing existing craters. The lesser internal warmth at Rhea could have resulted in fewer erasures or there could have been more bombardment on Rhea. Whatever the reason, Rhea is more heavily cratered than Dione and Tethys."[10]

"The Voyager images showed that Rhea's features could be divided into two regions: the first being heavily cratered (bright) terrain with craters larger than 25 miles (40 km) across and a second type of area in parts of the polar and equatorial region with craters less than 25 miles (40 km) across. This difference may indicate there was a major resurfacing event some time in Rhea's history. However, it would have been long ago because there are few young craters with rays extending away from them (as on Earth's Moon)."[10]

"The Voyager images also showed mysterious linear "wispy" lines with lengths of tens to hundreds of miles, often cutting through plains and craters. In 2006, Cassini spacecraft images showed that the wispy areas are subsidence fractures that make canyons (some of them several hundred meters high). The walls of those canyons are bright because darker material falls off them, exposing fresh bright water ice. These fracture cliffs show Rhea may have been tectonically active in its past. This type of surface feature also occurs on Dione and Tethys."[10]

"The Cassini spacecraft detected a very thin atmosphere known as an exosphere, infused with oxygen and carbon dioxide around Rhea in 2010. It was the first time a spacecraft directly captured molecules of an oxygen atmosphere ? albeit a very thin one -- at a world other than Earth."[10]

"The oxygen appears to arise when Saturn's magnetic field rotates over Rhea. Energetic particles trapped in the planet's magnetic field pepper the moon's water-ice surface. They cause chemical reactions that decompose the surface and release oxygen. The source of the carbon dioxide is less certain."[10]

"Oxygen at Rhea's surface is estimated to be about 5 trillion times less dense than what we have at Earth. But the new results show that surface decomposition could contribute abundant molecules of oxygen, leading to surface densities roughly 100 times greater than the exospheres of either Earth's moon or Mercury."[10]

"In 2008, the Cassini spacecraft found evidence of material orbiting Rhea--the first time rings had been found around a moon. A broad debris disk and at least one ring appear to have been detected by a suite of six instruments on Cassini specifically designed to study the atmospheres and particles around Saturn and its moons."[10]

Rings[edit | edit source]

Cassini instruments provide complementary information about the structure of Saturn's rings. Credit: NASA/JPL/Space Science Institute.

"Cassini instruments provide complementary information about the structure of Saturn's rings. Narrow and wide angle cameras provide images in the visible region of the electromagnetic, spectrum much like a digital camera does. The images have information about how the ring structure differs both with distance from the planet and with position around the equatorial circle. However, resolution is usually limited to few kilometers at best."[11]

"Radio and stellar occultations of the rings also provide important information about ring structure, but only along a one-dimensional track through the rings. The radial resolution can be as fine as 50 meters (164 feet). An "image" is then constructed by assuming circular symmetry over the ring region of interest. Color is usually added to encode other information related to the observed structure."[11]

"This image compares structure of Saturn's rings observed by these two approaches. The upper half is a natural color mosaic of images by the Cassini narrow-angle camera (see PIA06175). The bottom simulated images is constructed from a radio occultation observation conducted on May 3, 2005. Color in the lower image is used to represent information about ring particle sizes. For another view created using this process (see PIA07872)."[11]

Tethys[edit | edit source]

This image of Tethys is taken in visible green light with the Cassini spacecraft narrow-angle camera on September 14, 2011. Credit: NASA Cassini.
Voyager 2 imaged Tethys on August 25, 1981. Credit: NASA/JPL.
This is Tethys as imaged by Voyager 2. Credit: NASA/JPL.
This view from the Cassini orbital mission at Saturn shows the high-resolution color of the leading hemisphere of Tethys. Credit: NASA/JPL/Space Science Institute/Universities Space Research Association/Lunar & Planetary Institute.
An animation shows Tethys's surface. Credit: Brandon Amaro.

At right is an image of Saturn's moon Tethys in green light.

"On the top left of the image there is huge Odysseus Crater. See PIA07693 for a closer view. On the bottom right there is Ithaca Chasma, a series of scarps that runs north-south across the moon for more than 620 miles (1,000 kilometers). North on Tethys is up and rotated 25 degrees to the right."[12]

"This view looks toward the area between the leading hemisphere and Saturn-facing side of Tethys (660 miles, or 1,062 kilometers across)."[12]

"The image was taken in visible green light with the Cassini spacecraft narrow-angle camera on Sept. 14, 2011. The view was acquired at a distance of approximately 178,000 miles kilometers (287,000) from Tethys and at a Sun-Tethys-spacecraft, or phase, angle of 11 degrees. Image scale is about 1 mile (2 kilometers) per pixel."[12]

"Tethys shows two distinct types of terrain--bright, densely cratered regions; and relatively dark, lightly cratered planes that extend in a broad belt across the satellite. The densely cratered terrain is believed to be part of the ancient crust of the satellite; the lightly cratered planes are thought to have been formed later by internal processes. Also clearly seen is a trough that runs parallel to the terminator (the day-night boundary, seen at right). This trough is an extension of the huge canyon system Voyager 1 saw last fall. This system extends nearly two-thirds the distance around Tethys."[13]

At lower right "Tethys is shown here in a Voyager 2 image taken 26 August 1981 from 282,600 km away. Tethys is 1,060 km in diameter. Ithaca Chasma is a large canyon running diagonally in the left of this image; Ithaca Chasma is up to 100 km wide, several km deep, and stretches at least three-fourths of the distance around Tethys. "[14]

Fourth down on the right is the first global high-resolution color image of Tethys.

"The color map shows the prominent dusky bluish band along the equator, first seen by Voyager in 1980, and shown ... to be due to the bombardment and alteration of the surface by high energy electrons traveling slower than the satellite's revolution period."[15]

Thrymr[edit | edit source]

This shows the Saturnian moon Thrymr. Credit: Greece11.

"Thrymr has a mean radius of 2.2 miles (3.5 km), assuming an albedo (a measure of how reflective the surface is) of 0.06. It orbits Saturn at an inclination of about 174 degrees and an eccentricity of about 0.5. At a mean distance of 12.7 million miles (20.4 million km) from Saturn, the moon takes about 1,094 Earth days to complete one orbit."[16]

"Thrymr is a member of the Norse group of moons. These "irregular" moons have retrograde orbits around Saturn -- traveling around in the opposite direction from the planet's rotation. Thrymr and the other Norse moons also have eccentric orbits, meaning they are more elongated than circular."[16]

"Voyager 2 obtained this [upper right] image of Tethys on Aug. 25, when the spacecraft was 594,000 kilometers (368,000 miles) from this satellite of Saturn. This photograph was compiled from images taken through the violet, clear and green filters of Voyager's narrow-angle camera."[13]

Theoretical Saturn[edit | edit source]

"Planets are believed to have formed through the accumulation of a large number of small bodies1, 2, 3, 4. In the case of the gas-giant planets Jupiter and Saturn, they accreted a significant amount of gas directly from the protosolar nebula after accumulating solid cores of about 5–15 Earth masses5, 6. Such models, however, have been unable to produce the smaller ice giants7, 8 Uranus and Neptune at their present locations, because in that region of the Solar System the small planetary bodies will have been more widely spaced, and less tightly bound gravitationally to the Sun."[17]

"When applied to the current Jupiter–Saturn zone, a recent theory predicts that, in addition to the solid cores of Jupiter and Saturn, two or three other solid bodies of comparable mass are likely to have formed9. [Model calculations] demonstrate that such cores will have been gravitationally scattered outwards as Jupiter, and perhaps Saturn, accreted nebular gas. The orbits of these cores then evolve into orbits that resemble those of Uranus and Neptune, as a result of gravitational interactions with the small bodies in the outer disk of the protosolar nebula."[17]

In the gaseous protoplanetary disk, the "mutual interactions between Jupiter and Saturn prevented [...] migration from driving these planets much closer to the Sun."[18]

"After a phase of inward runaway migration, Saturn was captured into the 2:3 mean motion resonance with Jupiter. At that point, the planets reversed their migration, moving outward in parallel, while preserving their resonant relationship."[18]

"In fact, after Jupiter and Saturn lock in their mutual 2:3 resonance, their outward migration is rather fast. Jupiter increases its orbital radius by ∼40% in 1000 orbits. If this really occurred in the Solar System, Jupiter would have been at some time in the middle of the asteroid belt. The properties of the asteroid belt (in particular the quite tight zoning of the taxonomic types) exclude this possibility."[18]

The "migration reversal [...] does not depend on the history of the previous migration."[18]

Arguments "favor [...] a close formation of Saturn [...] The direction of migration of Jupiter determines the subsequent evolution of both planets, once they are locked in resonance. The planets have to move in parallel to preserve the resonant configuration."[18]

"In most cases, the planets migrate outward, which is not a viable evolution in our Solar System, because it would imply that Jupiter was in the asteroid belt in the past. However, there is a range of values of viscosity and disk’s scale height such that, once in resonance, the planets have a quasi-stationary evolution during which their semi-major axes remain practically constant. We argue that Jupiter and Saturn actually followed this kind of evolution."[18]

Astrognosy[edit | edit source]

Diagram is of the planet Saturn. Credit: Kelvinsong.

The internal structure of the gaseous giant Saturn is modeled on the right.

Electromagnetics[edit | edit source]

"The first systematic attempt to base a theory of the origin of the solar system on electromagnetic or hydromagnetic effects was made in Alfvén (1942). The reason for doing so was that a basic difficulty with the old Laplacian hypothesis: how can a central body (Sun or planet) transfer angular momentum to the secondary bodies (planets or satellites) orbiting around it? It was demonstrated that this could be done by electromagnetic effects. No other acceptable mechanism has yet been worked out. [...] the electromagnetic transfer mechanism has been confirmed by observations, as described in the monograph Cosmic Plasma (Alfvén, 1981, pp. 28, 52, 53 0."[19]

"If charged particles (electrons, ions or charged grains) move in a magnetic dipole field - strong enough to dominate their motion - under the action of gravitation and the centrifugal force, they will find an equilibrium in a circular orbit if their centrifugal force is 2/3 of the gravitational force [...] The consequence of this is that if they become neutralized, so that electromagnetic forces disappear, the centrifugal force is too small to balance the gravitation. Their circular orbit changes to an elliptical orbit with the semi-major axis a = 3/4a0 and e = 1/3 (where a0 is the central distance where the neutralization takes place [...] Collisional (viscous) interaction between the condensed particles will eventually change the orbit into a new circular orbit with a = 2/3a0 and e = 0."[19]

"If [...] there is plasma in the region [collisional interaction results in] matter in the 2/3-[region]. [...] matter in the region [...] will produce a [cosmogonic] shadow in the region".[19]

Weak forces[edit | edit source]

"Measurements taken by NASA's Cassini spacecraft have shown that the ringed planet might have a longer day than originally calculated from measurements taken by the Voyager 2 probe more than 20 years earlier."[20]

"While an uncertainty of 15 minutes may appear small compared to the approximately 10.5-hour rotation of Saturn, it is actually important to know [the rotation] accurately. The rotation period has an important effect on understanding Saturn's atmosphere dynamics and internal structure."[21]

"When Voyager 2 visited Saturn in 1981, the probe measured the planet's rotation period at about 10 hours, 39 minutes. But when Cassini first arrived at the planet in the early 2000s, it determined Saturn spun once on its axis every 10 hours and 47 minutes, and those numbers changed each time Cassini took a look."[20]

"Voyager and Cassini relied on measurements of the planet's radio radiation, but because those measurements shifted with each observation, they proved unreliable."[20]

"Radio radiation isn't the only method for studying the rotation of a gas giant. For planets where the magnetic field is tilted in relation to the axis the planet rotates around, measurements of the magnetic field can reveal how quickly the planet spins. However, Saturn's magnetic field lines up with its rotation axis, which prevents scientists from relying on that measure."[20]

"A third option involves measuring how long it takes for a cloud in Saturn's atmosphere to travel around the planet. But the rotation of the atmosphere doesn't necessarily line up with the rotation of the planet, making this method challenging."[20]

A "more mathematical approach [involves searching] for solutions for the rotation period by using coefficients to represent the interior, then [searching] for the rotation period that the most solutions calculated."[20]

"We did not want the derived period to be associated with a specific internal structure, so we accounted for many possibilities within their physical range. There are many solutions, but it was found that they tend to give a similar rotation period."[21]

"The theoretical estimate returned a rotation of almost 10 hours, 33 minutes."[20]

This is "in very good agreement with previous estimates that used different methods."[21]

"The newly returned calculation relied on studies of the planet's well-defined gravitational field. As Cassini traveled around the planet, it measured the tug of Saturn on the spacecraft, determining the strength or weakness of the gravitational pull."[20]

"The advantage of our method is that it is not associated with a specific interior model for Saturn, does not rely on the cloud-tracking wind properties that have large variability, and allows for the large range of solutions constrained by the measured physical properties of the planet and their uncertainties."[21]

"Saturn is rather thick around the middle, more than even Jupiter, which could indicate a fast spin. However, Helled pointed out that winds also affect oblateness, so strong winds around the equator could lead to a bigger bulge."[20]

"Such a rotation period for Saturn implies that the latitudinal wind structure is more symmetric, containing both easterly and westerly jets, like we see on Jupiter."[21]

Bands[edit | edit source]

Image of Saturn shows the square shadow where the planet's shadow meets the Cassini division. Credit: Mark and Nigel Stronge.

"The hydromagnetic approach led to the discovery of two important observational regularities in the solar system: (1) the band structure [such as in the rings of Saturn and in the asteroid belt], and (2) the cosmogonic shadow effect (the two-thirds fall down effect)."[19]

"Saturn's square shadow results in a similar fashion to the notorious 'black drop' effect observed during transits of the inferior planets, Mercury and Venus, across the face of the Sun."[22]

"It seems that the black drop is caused by a combination of telescopic or instrumental effects and the unsteadiness of the Earth's atmosphere, when observing the sharp, dark edge of a planet against the edge of a background source of light (the Sun)."[22]

"When Saturn's shadow falls on its rings near the principal gap, the Cassini division, the geometry and optical arrangement are such that the situation is the same as for the black drop effect, that is, a sharp planetary shadow meeting the abrupt edge of the bright background rings."[22]

Meteors[edit | edit source]

The huge storm (great white spot) churning through the atmosphere in Saturn's northern hemisphere overtakes itself as it encircles the planet in this true-color view from NASA’s Cassini spacecraft. Credit: NASA/JPL-Caltech/SSI.

A huge storm (great white spot) shown in the image on the right, churning through the atmosphere in Saturn's northern hemisphere overtakes its own trail in this true-color view from NASA’s Cassini spacecraft. Note that the trail of the disturbance in the atmosphere has apparently moved closer to the equator than the storm itself.

Equatorial storms[edit | edit source]

This NASA Hubble Space Telescope image of the ringed planet Saturn shows a rare storm that appears as a white arrowhead-shaped feature near the planet's equator. Credit: Reta Beebe, D. Gilmore, L. Bergeron, NASA.

In 1990, the Hubble Space Telescope imaged an enormous white cloud near Saturn's equator that was not present during the Voyager encounters and in 1994, another, smaller storm was observed. The 1990 storm was an example of a Great White Spot, a unique but short-lived phenomenon that occurs once every Saturnian year, roughly every 30 Earth years, around the time of the northern hemisphere's summer solstice.[23] Previous Great White Spots were observed in 1876, 1903, 1933 and 1960, with the 1933 storm being the most famous. If the periodicity is maintained, another storm will occur in about 2020.[24]

Wind speeds on Saturn can reach 1,800 km/h (1,100 mph) ... Voyager data indicate peak easterly winds of 500 m/s (1800 km/h).[25]

"This NASA Hubble Space Telescope image [fourth down on the right] of the ringed planet Saturn shows a rare storm that appears as a white arrowhead-shaped feature near the planet's equator. The storm is generated by an upwelling of warmer air, similar to a terrestrial thunderhead. The east-west extent of this storm is equal to the diameter of the Earth (about 7,900 miles). Hubble provides new details about the effects of Saturn's prevailing winds on the storm. The new image shows that the storm's motion and size have changed little since its discovery in September, 1994."[26]

"The storm was imaged with Hubble's Wide Field Planetary Camera 2 (WFPC2) in the wide field mode on December 1, 1994, when Saturn was 904 million miles from the Earth. The picture is a composite of images taken through different color filters within a 6 minute interval to create a "true-color" rendition of the planet. The blue fringe on the right limb of the planet is an artifact of image processing used to compensate for the rotation of the planet between exposures."[26]

"The Hubble images are sharp enough to reveal that Saturn's prevailing winds shape a dark "wedge" that eats into the western (left) side of the bright central cloud. The planet's strongest eastward winds (clocked at 1,000 miles per hour from analysis of Voyager spacecraft images taken in 1980-81) are at the latitude of the wedge."[26]

"To the north of this arrowhead-shaped feature, the winds decrease so that the storm center is moving eastward relative to the local flow. The clouds expanding north of the storm are swept westward by the winds at higher latitudes. The strong winds near the latitude of the dark wedge blow over the northern part of the storm, creating a secondary disturbance that generates the faint white clouds to the east (right) of the storm center."[26]

"The storm's white clouds are ammonia ice crystals that form when an upward flow of warmer gases shoves its way through Saturn's frigid cloud tops. This current storm is larger than the white clouds associated with minor storms that have been reported more frequently as bright cloud features."[26]

"Hubble observed a similar, though larger, storm in September 1990, [sixth image down on the right] which was one of three major Saturn storms seen over the past two centuries. Although these events were separated by about 57 years (approximately 2 Saturnian years) there is yet no explanation why they apparently follow a cycle -- occurring when it is summer in Saturn's northern hemisphere."[26]

Ring rains[edit | edit source]

This is a Hubble Space Telescope (HST) image of Saturn. Credit: NASA/ESA Hubble Space Telescope.

"[E]rosion from particles making up the icy rings of Saturn are forming rain water that falls on certain parts of the planet. ... tiny ice particles that compose the planet's distinctive rings are sometimes eroded away and then deposited in the planet's upper atmosphere. The droplets then create a kind of rain on the planet. ... charged water molecules rain down only on certain parts of the planet, which show up darker in infrared images. ... The magnetic connection creates a pathway for small ice particles in the rings to slough off into the planet's atmosphere, causing the "ring rain.""[27]

"The most surprising element to us was that these dark regions on the planet are found to be linked — via magnetic field lines — to the solid portions of water-ice within Saturn's ring-plane"[28].

"Saturn is the first planet to show significant interaction between its atmosphere and ring system ... The main effect of ring rain is that it acts to 'quench' the ionosphere of Saturn. In other words, this rain severely reduces the electron densities in regions in which it falls."[29]

"It turns out that a major driver of Saturn's ionospheric environment and climate across vast reaches of the planet are ring particles located some 36,000 miles [60,000 kilometers] overhead ... The ring particles affect both what species of particles are in this part of the atmosphere and where it is warm or cool."[30]

"Where Jupiter is glowing evenly across its equatorial regions, Saturn has dark bands where the water is falling in, darkening the ionosphere".[31]

North Polar Stratospheric Vortex[edit | edit source]

North polar hexagonal cloud feature, discovered by Voyager 1 and confirmed in 2006 by Cassini is shown. Credit: NASA / JPL-Caltech / Space Science Institute.
This is a closer view of the north polar vortex at the center of the hexagon. Credit: NASA / JPL-Caltech / Space Science Institute.
This colorful view from NASA's Cassini mission is the highest-resolution view of the unique six-sided jet stream at Saturn's north pole. Credit: Jia-Rui C. Cook/JPL and Dwayne Brown/NASA HQ.
The Cassini spacecraft captures three magnificent sights at once: Saturn's north polar vortex and hexagon along with its expansive rings. Credit: NASA/JPL-Caltech/Space Science Institute.

In the image down on the right, the "Cassini spacecraft captures three magnificent sights at once: Saturn's north polar vortex and hexagon along with its expansive rings."[32]

"The hexagon, which is wider than two Earths, owes its appearance to the jet stream that forms its perimeter. The jet stream forms a six-lobed, stationary wave which wraps around the north polar regions at a latitude of roughly 77 degrees North."[32]

"This view looks toward the sunlit side of the rings from about 37 degrees above the ringplane. The image was taken with the Cassini spacecraft wide-angle camera on April 2, 2014 using a spectral filter which preferentially admits wavelengths of near-infrared light centered at 752 nanometers."[32]

"The view was obtained at a distance of approximately 1.4 million miles (2.2 million kilometers) from Saturn and at a Sun-Saturn-spacecraft, or phase, angle of 43 degrees. Image scale is 81 miles (131 kilometers) per pixel."[32]

A persisting hexagonal wave pattern around the north polar vortex in the atmosphere at about 78°N was first noted in the Voyager images.[33][34]

"The longevity of the exploration of the Saturn system by Cassini allows the use of infrared spectroscopy to trace the formation of the North Polar Stratospheric Vortex (NPSV), a region of enhanced temperatures and elevated hydrocarbon abundances at millibar pressures."[35]

"Although the NPSV formed during late northern spring, by the end of Cassini’s reconnaissance (shortly after northern summer solstice), it still did not display the contrasts in temperature and composition that were evident at the south pole during southern summer. The newly formed NPSV was bounded by a strengthening stratospheric thermal gradient near 78°N. The emergent boundary was hexagonal, suggesting that the Rossby wave responsible for Saturn’s long-lived polar hexagon—which was previously expected to be trapped in the troposphere—can influence the stratospheric temperatures some 300 km above Saturn’s clouds."[35]

"Composite Infrared Spectrometer (CIRS)27 reveal a significant surprise: the NPSV exhibits a hexagonal boundary that mirrors the well-studied hexagonal wave in Saturn’s troposphere28,29,30. The meandering of the jet that forms the hexagon is believed to be a Rossby wave31 resulting from an instability of the eastward zonal jet near 78°N29,32,33,34 and trapped within a waveguide formed by the zonal jets and Saturn’s vertical static stability profile."[35]

"Saturn’s famous hexagon is not always restricted to the troposphere but can persist high in the stratosphere in the spring/summer, creating a hexagonal structure that spans more than ~300 km in height from the clouds to the stratospheric polar vortex."[35]

The "tropospheric hexagon vertices do not move with the ~120 ms−1 eastward cloud-top velocity of the jet at 78°N".[35]

"Using the sinusoidal fits, [there is] a westward shift in the tropospheric hexagon vertices of 8.5 ± 1.1° over 963 days (the uncertainty comes from the quality of the sinusoidal fit). Offsets between the tropospheric and stratospheric vertices were <4° in February 2017."[35]

"Most surprisingly, the boundary of the NPSV exhibited a hexagonal shape mirroring that observed in the clouds ~300 km below."[35]

Subsidence "is occurring within the hexagon and that it extends from the cloud-forming region into the mid-stratosphere. In addition, the polar region exhibits an increased optical thickness of stratospheric hazes47,54 that is potentially related to aerosol production associated with Saturn’s aurora. Saturn’s main auroral oval, associated with the boundary between open and closed magnetic field lines, occurs at an average latitude of 76.5°N55 and therefore completely encompasses the area of the NPSV, sitting ~1° south of the hexagon latitude (78°N)."[35]

Hurricane-like vortex at the south pole[edit | edit source]

Cassini stares deep into the swirling hurricane-like vortex at Saturn's south pole, where the vertical structure of the clouds is highlighted by shadows. Credit: NASA.

In the image down on the right "Cassini stares deep into the swirling hurricane-like vortex at Saturn's south pole, where the vertical structure of the clouds is highlighted by shadows. Such a storm, with a well-developed eye ringed by towering clouds, is a phenomenon never before seen on another planet."[36]

The image "shows a swirling cloud mass centered on the south pole, around which winds blow at 550 kilometers (350 miles) per hour. [...] The clouds inside the dark, inner circle are lower than the surrounding clouds, which cast a shadow that follows the sun."[36]

"The width of the shadow and the height of the sun above the local horizon yield a crude estimate of the height of the surrounding clouds relative to the clouds in the center. The shadow-casting clouds tower 30 to 75 kilometers (20 to 45 miles) above those in the center. This is two to five times greater than the tallest terrestrial thunderstorms and two to five times the height of clouds surrounding the eye of a terrestrial hurricane. Such a height difference arises because Saturn's hydrogen-helium atmosphere is less dense at comparable pressures than Earth's atmosphere, and is therefore more distended in the vertical dimension."[36]

"The south polar storm, which displays two spiral arms of clouds extending from the central ring and spans the dark area inside a thick, brighter ring of clouds, is approximately 8,000 kilometers (5,000 miles) across, which is considerably larger than a terrestrial hurricane."[36]

"Eye-wall clouds are a distinguishing feature of hurricanes on Earth. They form where moist air flows inward across the ocean's surface, rising vertically and releasing a load of precipitation around an interior circular region of descending air, which is the eye itself."[36]

"Though it is uncertain whether moist convection is driving this storm, as is the case with Earthly hurricanes, the dark 'eye' at the pole, the eye-wall clouds and the spiral arms together indicate a hurricane-like system. The distinctive eye-wall clouds especially have not been seen on any planet beyond Earth. Even Jupiter's Great Red Spot, much larger than Saturn's polar storm, has no eye, no eye-wall, and is relatively calm at the center."[36]

"This giant Saturnian storm is apparently different from hurricanes on Earth because it is locked to the pole, does not drift around like terrestrial hurricanes and because it does not form over liquid water oceans."[36]

"The images were acquired over a period of three hours on Oct. 11, 2006, when Cassini was approximately 340,000 kilometers (210,000 miles) from Saturn. Image scale is about 17 kilometers (11 miles) per pixel. The images were taken with the wide-angle camera using a spectral filter sensitive to wavelengths of infrared light centered at 752 nanometers. All frames have been contrast enhanced using digital image processing techniques. The unprocessed images show an oblique view toward the pole, and have been reprojected to show the planet from a perspective directly over the south pole."[36]

The upper clouds are composed of ammonia crystals.

Infrared imaging has shown that Saturn's south pole has a warm polar vortex, the only known example of such a phenomenon in the Solar System.[37] Whereas temperatures on Saturn are normally −185 °C, temperatures on the vortex often reach as high as −122 °C, believed to be the warmest spot on Saturn.[37]

Electrons[edit | edit source]

"[M]agnetospheric electron (bi-directional) beams connect to the expected locations of Saturn’s aurora".[38]

X-rays[edit | edit source]

An X-ray astronomy image of Saturn is compared here with the optical image in the visible. Credit: X-ray: NASA/U. Hamburg/J. Ness et al; Optical: NASA/STScI.
In this image the rings of Saturn sparkle in X-rays. Credit: NASA/CXC/SAO.

The X-ray astronomy image of Saturn is on the left in the composite at right. The Chandra X-ray Observatory "image of Saturn held some surprises for the observers. First, Saturn's 90 megawatts of X-radiation is concentrated near the equator. This is different from a similar gaseous giant planet, Jupiter, where the most intense X-rays are associated with the strong magnetic field near its poles. Saturn's X-ray spectrum, or the distribution of its X-rays according to energy, was found to be similar to that of X-rays from the Sun. This indicates that Saturn's X-radiation is due to the reflection of solar X-rays by Saturn's atmosphere. The intensity of these reflected X-rays was unexpectedly strong. ... The optical image of Saturn is also due to the reflection of light from the Sun - visible wavelength light in this case - but the optical and X-ray images obviously have dramatic differences. The optical image is much brighter, and shows the beautiful ring structures, which were not detected in X-rays. This is because the Sun emits about a million times more power in visible light than in X-rays, and X-rays reflect much less efficiently from Saturn's atmosphere and rings."[39]

"[T]he soft X-ray emissions of Jupiter (and Saturn) can largely be explained by scattering and fluorescence of solar X-rays."[40]

The second image at the right, "taken by the Chandra x-ray telescope, reveals that the rings of Saturn sparkle; in this x-ray/optical composite, they are visible as blue dots. This radiation’s source is likely fluorescence caused by solar x-rays as they strike oxygen atoms in the water molecules of the planet’s icy rings. As the image shows, most of the ring’s x-rays originate in the B ring—the bright white inner ring visible in this optical image—which is approximately 25,000 kilometers wide and 40,000 kilometers above the planet’s surface. X-rays may also be concentrated on Saturn’s left side, possibly because of their association with shadows in the planet’s rings that are known as spokes, or possibly as a result of the additional solar fluorescence caused by the transient ice clouds that produce spokes. Other Chandra observations of Saturn show that the x-ray brightness of the rings varies significantly from one week to the next."[41]

Ultraviolets[edit | edit source]

This image of Saturn is taken in ultraviolet light. Credit: NASA and E. Karkoschka (University of Arizona).
This is a movie of Saturn in the ultraviolet from the Hubble Space Telescope. Credit: NASA, ESA, and Jonathan Nichols (University of Leicester).
Saturnian aurora whose Lyman alpha false reddish colour in this image is characteristic of ionized hydrogen plasma. Credit: J. Trauger (JPL), NASA.
This is an image of Saturn's A Ring, taken by the Cassini Orbiter using an Ultraviolet Imaging Spectrograph. Credit: NASA/JPL/University of Colorado.

"One of a series, this image [at right] of Saturn was taken when the planet's rings were at their maximum tilt of 27 degrees toward Earth. Saturn experiences seasonal tilts away from and toward the sun, much the same way Earth does. This happens over the course of its 29.5-year orbit. Every 30 years, Earth observers can catch their best glimpse of Saturn's south pole and the southern side of the planet's rings. ... NASA's Hubble Space Telescope [captured detailed images of Saturn's Southern Hemisphere and the southern face of its rings."[42]

The movie at right records Saturn "when its rings were edge-on, resulting in a unique movie featuring the nearly symmetrical light show at both of the giant planet's poles. It takes Saturn almost thirty years to orbit the Sun, with the opportunity to image both of its poles occurring only twice during that time. The light shows, called aurorae, are produced when electrically charged particles race along the planet's magnetic field and into the upper atmosphere where they excite atmospheric gases, causing them to glow. Saturn's aurorae resemble the same phenomena that take place at the Earth's poles."[43]

Powered by the Saturnian equivalent of (filamentary) Birkeland currents, streams of charged particles from the interplanetary medium interact with the planet's magnetic field and funnel down to the poles.[44] Double layers are associated with (filamentary) currents,[45][46] and their electric fields accelerate ions and electrons.[47]

"Towering more than 1,000 miles above the cloud tops, these Saturnian auroral displays are analogous to Earth's. ... In this false color image, the dramatic red aurora identify emission from atomic hydrogen, while the more concentrated white areas are due to hydrogen molecules."[48]

"The best view of Saturn's rings in the ultraviolet indicates there is more ice toward the outer part of the rings, than in the inner part, hinting at the origins of the rings and their evolution."[49]

"Images taken during the Cassini spacecraft's orbital insertion on June 30 show compositional variation in the A, B and C rings. From the inside out, the "Cassini Division" in faint red at left is followed by the A ring in its entirety. The Cassini Division at left contains thinner, dirtier rings than the turquoise A ring, indicating a more icy composition. The red band roughly three-fourths of the way outward in the A ring is known as the Encke gap."[49]

"The ring system begins from the inside out with the D, C, B and A rings followed by the F, G and E rings. The red in the image indicates sparser ringlets likely made of "dirty," and possibly smaller, particles than in the icier turquoise ringlets."[49]

The image at right "was taken with the Ultraviolet Imaging Spectrograph instrument, which is capable of resolving the rings to show features up to 97 kilometers (60 miles) across, roughly 100 times the resolution of ultraviolet data obtained by the Voyager 2 spacecraft."[49]

The image at second left Saturn's northern UV auroras. These exhibit changes in shape over the course of the observing interval.

"Saturn’s magnetosphere -- the big magnetic bubble that surrounds the planet -- is compressed on the side facing the sun, and it streams out into a long “magnetotail” on the planet’s nightside. Just like with comets, the magnetotails of Earth and Saturn are made of electrified gas from the sun."[50]

"Now it appears that when strong bursts of particles from the sun hit Saturn, the magnetotail collapses and then reconfigures itself -- a disturbance of the magnetic field that’s reflected in the dynamics of auroras."[50]

“We have always suspected this was what also happens on Saturn. This evidence really strengthens the argument.”[51]

“We can see that the magnetotail is undergoing huge turmoil and reconfiguration, caused by buffering from solar wind. It’s the smoking gun that shows us that the tail is collapsing.”[51]

Opticals[edit | edit source]

This image of Saturn was taken with the 2.6 meter Nordic Optical Telescope, located at La Palma, Canary Islands. Credit: Nordic Optical Telescope Scientific Association.

The image on the right of Saturn was taken with the 2.6 meter Nordic Optical Telescope, located at La Palma, Canary Islands.

The optical image shows the blue color of Saturn's northern hemisphere.

Visuals[edit | edit source]

This image from NASA's Hubble Space Telescope shows Saturn's Southern Hemisphere and the southern face of its rings in visible light. Credit: NASA/ESA and E. Karkoschka (University of Arizona).

"This image from NASA's Hubble Space Telescope shows Saturn's Southern Hemisphere and the southern face of its rings in visible light."[52]

"Saturn experiences seasonal tilts away from and toward the Sun, much the same way Earth does, over the course of its 29.5-year orbit. This means that approximately every 30 years, we can catch Saturn with its rings at their maximum tilt of 27 degrees toward Earth and get the best glimpse of Saturn's South Pole and the southern side of the planet's rings."[52]

Violets[edit | edit source]

This view from Voyager 2 is of Saturn's north polar region through the orange and violet filters. Credit: NASA/JPL.
The image shows a subtle northward gradation from gold to azure on Saturn. Credit: NASA/JPL.

"The north polar region of Saturn is pictured in great detail in this Voyager 2 image obtained Aug. 25 from a range of 633,000 kilometers (393,000 miles)."[53]

"Two oval cloud systems some 250 km (150 mi) across are visible at about 72 degrees north latitude. The bright spot in the center of the leftmost cloud is a convective cloud storm about 60 km. (37 mi.)across. The outer ring of material rotates in an anti-cyclonic sense(counterclockwise in the northern hemisphere). A similar cloud structure of comparable dimension appears at 55 degrees north (bottom center of this picture). These northern latitudes contain many bright, small-scale cloud spots--only a few tens of kilometers across--representative of convective cloud systems. Across the top of this image stretch several long, linear, wavelike features that may mark the northernmost east-flowing jet in Saturn's atmosphere."[53]

"In this orange-and-violet-image composite, the smallest features visible are about 16 km. (10 mi.) across."[53]

In the second image at right, "[t]he gas planet's subtle northward gradation from gold to azure is a striking visual effect that scientists don't fully understand. Current thinking says that it may be related to seasonal influences, tied to the cold temperatures in the northern (winter) hemisphere. Despite Cassini's revelations, Saturn remains a world of mystery."[54]

Blues[edit | edit source]

Saturn's northern hemisphere is presently a serene blue as seen in this natural color image from Cassini. Credit: NASA/JPL/Space Science Institute.
The image shows Saturn's northern hemisphere from the Cassini spacecraft with Mimas in front. Credit: NASA/JPL/Space Science Institute.

"Saturn's northern hemisphere [as shown in the first image on the right] is presently a serene blue [...] as seen in this natural color image from Cassini."[55]

"Images obtained using red, green and blue spectral filters were combined to create this color view. The images were taken with the Cassini spacecraft wide angle camera on Dec. 14, 2004, at a distance of 719,200 kilometers (446,900 miles) from Saturn. The image scale is about 39 kilometers (24 miles) per pixel."[55]

In the image second down on the right, "Mimas drifts along in its orbit against the azure backdrop of Saturn's northern latitudes in this true color view from NASA's Cassini spacecraft. The long, dark lines on the atmosphere are shadows cast by the planet's rings."[56]

Cyans[edit | edit source]

The view of Saturn from Hubble, taken on March 22, 2004, is so sharp that many individual Saturnian ringlets can be seen. Credit: NASA, ESA and Erich Karkoschka (University of Arizona).

"The view [at right] from Hubble [of Saturn], taken on March 22, 2004, is so sharp that many individual Saturnian ringlets can be seen."[57]

"Hubble's exquisite optics, coupled with the high resolution of its Advanced Camera for Surveys, allow it to take pictures of Saturn which are nearly as sharp as Cassini's, even though Hubble is nearly a billion miles farther from Saturn than Cassini."[57]

"Camera exposures in four filters (blue, blue-green, green, and red) were combined to form the Hubble image, to render colors similar to what the eye would see through a telescope focused on Saturn. The subtle pastel colors of ammonia-methane clouds trace a variety of atmospheric dynamics. Saturn displays its familiar banded structure, and haze and clouds of various altitudes. Like Jupiter, all bands are parallel to Saturn's equator. Even the magnificent rings, at nearly their maximum tilt toward Earth, show subtle hues, which indicate the trace chemical differences in their icy composition."[57]

Cyans[edit | edit source]

The image of Saturn shows some greens. Credit: E. Karkoschka (University of Arizona).
The Saturn picture, released today, marks the first time Cassini captured a backlit view of the ringed planet since 2006. Credit: Carolyn Porco NASA / JPL-Caltech / SSI.

The image on the right shows natural greens in some of Saturn's bands and towards its edges from the Hubble Space Telescope.

"Saturn and its rings glow in a backlit, enhanced-color image [second image down on the right] from the Cassini orbiter. The picture combines images that were acquired using infrared, red and violet filters on Oct. 17. Two of Saturn's moons, Enceladus and Tethys, sparkle on the left side of the planet."[58]

"The Saturn picture, released today, marks the first time Cassini captured a backlit view of the ringed planet since 2006. That earlier photo made a huge splash, in part because the planet Earth could just barely be seen as a pale blue dot off to the side. This time, Earth is hidden behind Saturn, but you can spot two moons just to the left and below the planet: The closer speck is Enceladus, and Tethys is farther down and to the left."[58]

"The last time Cassini had such an unusual perspective on Saturn and its rings, at sufficient distance and with sufficient time to take a full mosaic of images of the entire system, occurred in September 2006 when it captured a mosaic of images, processed to look like natural color, entitled "In Saturn's Shadow-The Pale Blue Dot"."[59]

"The mosaic we are releasing today [18 December 2012] does not contain Earth: Along with the sun, our planet is hidden behind Saturn. However, it was taken when Cassini was closer to Saturn and therefore shows more detail in the rings than the one from six years ago. It also is displayed as it truly is, in false-color ... leaving a rather eerie and surreal impression on the viewer."[59]

Yellows[edit | edit source]

This is a Cassini image in natural color of the gaseous object Saturn. Credit: NASA/JPL/Space Science Institute.

The planet exhibits a pale yellow hue due to ammonia crystals in its upper atmosphere. Its exterior is predominantly composed of gas and it lacks a definite surface. The planet primarily consists of hydrogen. The outer atmosphere of Saturn contains 96.3% molecular hydrogen and 3.25% helium.[60] The proportion of helium is significantly deficient compared to the abundance of this element in the Sun.[61] Trace amounts of ammonia, acetylene, ethane, propane, phosphine and methane have been detected in Saturn's atmosphere.[62][63][64]

Oranges[edit | edit source]

This is an Earth-based telescopic observation pre-1979 of Saturn which shows its subdued browns. Credit: Hans-Peter Engel and Steve Garber, NASA.
The looming shape of Saturn stretches across this picture taken by Voyager 1 from 13 million kilometers (8 million miles) away. Credit: Hans-Peter Engel and Steve Garber, NASA.
A swing high above Saturn by NASA's Cassini spacecraft revealed this stately view of the planet and its main rings. The view is in natural colour, as human eyes would have seen it. Credit: NASA/JPL-Caltech/SSI/Cornell.

Early telescopic observations, i.e. pre-1979, as shown on the right revealed subdued browns of Saturn's upper atmosphere.

Later images from Pioneer 11 and Voyager 1 as the image on the left shows also exhibited subdued browns.

"A swing high above Saturn by NASA's Cassini spacecraft revealed this stately view of the golden-hued planet and its main rings. The view is in natural color, as human eyes would have seen it. This mosaic was made from 36 images in three color filters obtained by Cassini's imaging science subsystem on Oct. 10, 2013. The observation and resulting image mosaic were planned as one of three images for Cassini's 2013 Scientist for a Day essay contest."[65]

"Saturn sports differently colored bands of weather in this image [second down on the right]. For instance, a bright, narrow wave of clouds around 42 degrees north latitude appears to be some of the turbulent aftermath of a giant storm that reached its violent peak in early 2011. The mysterious six-sided weather pattern known as the hexagon is visible around Saturn's north pole."[65]

"When Cassini arrived in 2004, more of the northern hemisphere sported a bluish hue and it was northern winter. The golden tones dominated the southern hemisphere, where it was southern summer. But as the seasons have turned and northern spring is in full swing, the colors have begun to change in each hemisphere as well. Golden tones have started to dominate in the northern hemisphere and the bluish color in the north is now confined to a tighter circle around the north pole. The southern hemisphere has started getting bluer, too."[65]

Infrareds[edit | edit source]

This is Saturn imaged with the Stockholm Infrared Camera (SIRCA) in the H2O band. Credit: M. Gålfalk, G. Olofsson and H.-G. Florén, Nordic Optical Telescope.
This is a mosaic of 35 individual exposures taken with infrared radiation. Credit: NASA.
This is a false-color composite taken in the infrared of Saturn's south polar region. Credit: NASA/JPL/University of Arizona/University of Leicester.
This is an infrared image of Saturn's north pole. Credit: Cassini VIMS Team, University of Arizona, JPL, ESA and NASA.
This false-color mosaic shows Saturn's north polar region in infrared from the unlit side. Credit: NASA/JPL/University of Arizona.
This image of Saturn is in the infrared. Credit: NASA/E. Karkoschka (University of Arizona).
These infrared false-colour images from NASA's Cassini spacecraft chronicle a day in the life of a huge storm that developed from a small spot that appeared 12 weeks earlier in Saturn's northern mid-latitudes. Credit: NASA/JPL-Caltech/SSI.
Thermal infrared images of Saturn from the VISIR instrument on ESO’s VLT (centre and right) and an amateur visible-light image (left) from Trevor Barry (Broken Hill, Australia) obtained on 19 January 2011 during the mature phase of the northern storm. Credit: ESO/University of Oxford/L. N. Fletcher/T. Barry.
This is a Gemini North infrared image of Saturn and Titan (at about 6 o'clock position). Credit: Gemini Observatory/AURA/Henry Roe, Lowell Observatory/Emily Schaller, Insitute for Astronomy, University of Hawai‘i.

On the left is Saturn imaged by the Stockholm Infrared Camera (SIRCA) in the H2O infrared band to show the presence of water vapor. The image is cut off near the top due to the presence of Saturn's rings.

At right is an infrared astronomy image of Saturn. "This is the sharpest image of Saturn's temperature emissions taken from the ground; it is a mosaic of 35 individual exposures made at the W.M. Keck I Observatory, Mauna Kea, Hawaii on Feb. 4, 2004. The images to create this mosaic were taken with infrared radiation. The black square at 4 o'clock represents missing data."[66]

"In the most precise reading of Saturn's temperatures ever taken from Earth, a new set of infrared images suggests a warm "polar vortex" at Saturn's south pole - the first warm polar cap ever to be discovered in the solar system. The vortex is punctuated by a compact spot that is the warmest place on the planet."[66]

"The puzzle isn't that Saturn's south pole is warm; after all, it has been exposed to 15 years of continuous sunlight, having just reached its summer Solstice late in 2002. But both the distinct boundary of a warm polar vortex some 30 degrees latitude from the southern pole and a very hot "tip" right at the pole were completely unexpected. If the increased southern temperatures are the result of the seasonal variations of sunlight, then temperatures should increase gradually with increasing latitude. But they don't – the tropospheric temperature increases toward the pole abruptly near 70 degrees latitude from 88 to 89 Kelvin (- 301 to -299 degrees Fahrenheit) and then to 91 Kelvin (-296 degrees Fahrenheit) right at the pole. Near 70 degrees latitude, the stratospheric temperature increases even more abruptly from 146 to 150 Kelvin (-197 to -189 degrees Fahrenheit) and then again to 151 Kelvin (-188 degrees Fahrenheit) right at the pole."[66]

The second image at right is "constructed from data collected in the near-infrared wavelengths of light, the auroral emission is shown in green. The data represents emissions from hydrogen ions in of light between 3 and 4 microns in wavelength. In general, scientists designated blue to indicate sunlight reflected at a wavelength of 2 microns, green to indicate sunlight reflected at 3 microns and red to indicate thermal emission at 5 microns. Saturn's rings reflect sunlight at 2 microns, but not at 3 and 5 microns, so they appear deep blue. Saturn's high altitude haze reflects sunlight at both 2 and 3 microns, but not at 5 microns, and so it appears green to blue-green. The heat emission from the interior of Saturn is only seen at 5 microns wavelength in the spectrometer data, and thus appears red. The dark spots and banded features in the image are clouds and small storms that outline the deeper weather systems and circulation patterns of the planet. They are illuminated from underneath by Saturn's thermal emission, and thus appear in silhouette. The composite image was made from 65 individual observations by Cassini's visual and infrared mapping spectrometer on 1 November 2008. The observations were each six minutes long."[67]

The third image at right shows Saturn's northern polar region with "the aurora and underlying atmosphere, seen at two different wavelengths of infrared light as captured by NASA's Cassini spacecraft. Energetic particles, crashing into the upper atmosphere cause the aurora, shown in blue, to glow brightly at 4 microns (six times the wavelength visible to the human eye). The image shows both a bright ring, as seen from Earth, as well as an example of bright auroral emission within the polar cap that had been undetected until the advent of Cassini. This aurora, which defies past predictions of what was expected, has been observed to grow even brighter than is shown here. Silhouetted by the glow (cast here to the color red) of the hot interior of Saturn (clearly seen at a wavelength of 5 microns, or seven times the wavelength visible to the human eye) are the clouds and haze that underlie this auroral region."[68]

Also on the right is a fourth image of Saturn's north polar region in infrared. "This striking false-color mosaic was created from 25 images taken by Cassini's visual and infrared mapping spectrometer over a period of 13 hours, and captures Saturn in nighttime and daytime conditions. The visual and infrared mapping spectrometer acquires data simultaneously at 352 different wavelengths, or spectral channels. Data at wavelengths of 2.3, 3.0 and 5.1 microns were combined in the blue, green and red channels of a standard color image, respectively, to make this false-color mosaic."[69]

"This image was acquired on 24 February 2007, while the spacecraft was 1.58 million km (1 million miles) from the planet and 34.6 degrees above the ring plane. The solar phase angle was 69.5 degrees. In this view, Cassini was looking down on the northern, unlit side of the rings, which are rendered visible by sunlight filtering through from the sunlit, southern face."[69]

"On the night side (right side of image), with no sunlight, Saturn's own thermal radiation lights things up. This light at 5.1 microns wavelength (some seven times the longest wavelength visible to the human eye) is generated deep within Saturn, and works its way upward, eventually escaping into space. Thick clouds deep in the atmosphere block that light. An amazing array of dark streaks, spots and globe-encircling bands is visible instead. Saturn's strong thermal glow at 5.1 microns even allows these deep clouds to be seen on portions of the dayside (left side), especially where overlying hazes are thin and the glint of the sun off of them is minimal. These deep clouds are likely made of ammonium hydrosulfide and cannot be seen in reflected light on the dayside, since the glint of the sun on overlying hazes and ammonia clouds blocks the view of this level."[69]

"A pronounced difference in the brightness between the northern and southern hemispheres is apparent. The northern hemisphere is about twice as bright as the southern hemisphere. This is because high-level, fine particles are about half as prevalent in the northern hemisphere as in the south. These particles block Saturn's glow more strongly, making Saturn look brighter in the north."[69]

"At 2.3 microns (shown in blue), the icy ring particles are highly reflecting, while methane gas in Saturn's atmosphere strongly absorbs sunlight and renders the planet very dark. At 3.0 microns (shown in green), the situation is reversed: water ice in the rings is strongly absorbing, while the planet's sunlit hemisphere is bright. Thus the rings appear blue in this representation, while the sunlit side of Saturn is greenish-yellow in color. Within the rings, the most opaque parts appear dark, while the more translucent regions are brighter. In particular, the opaque, normally-bright B ring appears here as a broad, dark band separating the brighter A (outer) and C (inner) rings."[69]

"At 5.1 microns (shown in red), reflected sunlight is weak and thus light from the planet is dominated by thermal (i.e., heat) radiation that wells up from the planet's deep atmosphere. This thermal emission dominates Saturn's dark side as well as the north polar region (where the hexagon is again visible) and the shadow cast by the A and B rings. Variable amounts of clouds in the planet's upper atmosphere block the thermal radiation, leading to a speckled and banded appearance, which is ever-shifting due to the planet's strong winds."[69]

The fifth infrared image of Saturn is a detailed false color image. "[T]aken in January 1998 by the Hubble Space Telescope [it] shows the ringed planet in reflected infrared light. Different colors [indicate] varying heights and compositions of cloud layers generally thought to consist of ammonia ice crystals. The eye-catching rings cast a shadow on Saturn's upper hemisphere, while the bright stripe seen within the left portion of the shadow is infrared sunlight streaming through the large gap in the rings known as the Cassini Division."[70]

"Two of Saturn's many moons have also put in an appearance (in the full resolution version), Tethys just beyond the planet's disk at the upper right, and Dione at the lower left."[70]

The panoramic images at right "from NASA's Cassini spacecraft chronicle a day in the life of a huge storm that developed from a small spot that appeared 12 weeks earlier in Saturn's northern mid-latitudes."[71]

"This storm is the largest and most intense observed on Saturn by NASA's Voyager or Cassini spacecraft. The storm is still active. As seen in these and other Cassini images, the storm encircles the planet - whose circumference at these latitudes is 300,000 kilometres. From north to south, it covers a distance of about 15,000 kilometres, which is one-third of the way around the Earth. It encompasses an area of 4 billion square kilometres, or eight times the surface area of Earth. This storm is about 500 times the area of the biggest of the southern hemisphere storms ... observed by Cassini."[71]

"The highest clouds in the image are probably around 100 millibars pressure, 100 kilometres above the regular undisturbed clouds. These false colors show clouds at different altitudes. Clouds that appear blue here are the highest and are semitransparent, or optically thin. Those that are yellow and white are optically thick clouds at high altitudes. Those shown green are intermediate clouds. Red and brown colors are clouds at low altitude unobscured by high clouds, and the deep blue color is a thin haze with no clouds below. The base of the clouds, where lightning is generated, is probably in the water cloud layer of Saturn's atmosphere. The storm clouds are likely made out of water ice covered by crystallized ammonia."[71]

"Taken about 11 hours -- or one Saturn day -- apart, the two mosaics in the lower half of this image product consist of 84 images each. The mosaic in the middle was taken earlier than the mosaic at the bottom. Both mosaics were captured on Feb. 26, 2011, and each of the two batches of images was taken over about 4.5 hours."[71]

"Two enlargements from the earlier, middle mosaic are shown at the top of this product. The white lines below the middle mosaic identify those parts of the mosaic that were enlarged for these close-up views. The enlargement on the top left shows the head of the storm, and that on the top right shows the turbulent middle of the storm. Cassini observations have shown the head of the storm drifting west at a rate of about 2.8 degrees of longitude each Earth day (28 meters per second, or 63 miles per hour). The central latitude of the storm is the site of a westward jet, which means that the clouds to the north and south are drifting westward more slowly or even drifting eastward. In contrast, clouds at Saturn's equator drift eastward at speeds up to 450 meters per second (1,000 miles per hour). "[71]

"Both of the long mosaics cover an area ranging from about 30 degrees north latitude to 51 degrees north latitude. The views stretch from about 138 degrees west longitude on the left to 347 degrees west longitude on the right, passing through 360/0 degrees west longitude near the far right of the mosaics."[71]

"The images were taken with the Cassini spacecraft narrow-angle camera using a combination of spectral filters sensitive to wavelengths of near-infrared light. The images filtered at 889 nanometers are projected as blue. The images filtered at 727 nanometers are projected as green, and images filtered at 750 nanometers are projected as red."[71]

"The views were acquired at a distance of approximately 2.4 million kilometres from Saturn and at a sun-Saturn-spacecraft angle (phase angle) of 62 degrees. Both the top and bottom images are simple cylindrical map projections, defined such that a square pixel subtends equal intervals of latitude and longitude. At higher latitudes, the pixel size in the north-south direction remains the same, but the pixel size in the east-west direction becomes smaller. The pixel size is set at the equator, where the distances along the sides are equal. The images of the long mosaics have a pixel size of 53 kilometres at the equator, and the two close-up views have a pixel size of 9 kilometres per pixel at the equator."[71]

The seventh image down on the right shows thermal "infrared images of Saturn from the VISIR instrument on ESO’s VLT (centre and right) and an amateur visible-light image (left) from Trevor Barry (Broken Hill, Australia) obtained on 19 January 2011 during the mature phase of the northern storm. The second image is taken at a wavelength that reveals the structures in Saturn’s lower atmosphere, showing the churning storm clouds and the central cooler vortex. The third image is sensitive to much higher altitudes in Saturn’s normally peaceful stratosphere, where we see the unexpected beacons of infrared emission flanking the central cool region over the storm."[72] The two wavelengths are 18 µm and 8.6 µm.[72]

The eighth image down on the right shows a "Gemini North infrared image of Saturn and Titan (at about 6 o'clock position). Image obtained on May 7, 2009 (5:31 UTC) using the Altair adaptive optics system with the Near-infrared imager (NIRI). At the perimeter of Saturn's ring the F-ring is faintly visible. The F-ring was discovered in images from the Pioneer 11 spacecraft in 1979 and is normally not apparent in images taken with ground-based telescopes. Also apparent are several of Saturn's smaller moons. This color composite image made using data from three infrared filters (K' [2.0-2.1 microns], h210 [2.12 micron narrowband], and bracket gamma[2.17 micron narrowband]), the field of view is about 40 arcseconds across."[73]

Submillimeters[edit | edit source]

"[T]he PH3 1-0 rotational line (266.9 GHz) line [has been detected] in [the atmosphere of] Saturn".[74]

Radars[edit | edit source]

In the fall of 1999 and 2000, the rings of Saturn were imaged using the Arecibo S-band radar system. Credit: P. Nicholson, D. Campbell, R. French, G. Black and J.-L. Margot.

"Very low values of the radio brightness temperatures of the rings of Saturn indicate that their high radar reflectivity is not simply due to a gain effect in the backscatter direction. These two sets of observations are consistent with the ring particles having a very high single scattering albedo at radio wavelengths with multiple scattering effects being important. Comparison of scattering calculations for ice and silicate particles with radio and radar observations imply a mean particle radius of ~ 1 cm. [...] The inferred mean size is consistent with a model in which meteoroid impacts have caused a substantial reduction in the mean particle size from its initial value."[75]

"The image shown [on the right top] is a sum of 5 days of dual-circular polarization data, co-adding both polarizations. The Keplerian velocity profile of the rings results in the outermost or A ring which provides the earliest echo, appearing at a lower Doppler shift than the middle or B ring. This leads to four bright crossover regions on either side where signal from the two different rings add together, analogous to the north/south ambiguity for radar imaging of rigidly rotating bodies. A pronounced azimuthal asymmetry can be seen: the rings are brighter on the far quadrant on the receding (western) ansa than on the near quadrant of the approaching (eastern) ansa. The most widely accepted explanation of the asymmetry involves gravitational wakes generated by individual large ring particles, which are distorted by Keplerian shear into elongated structures trailing at angles of about 70 degrees from the radial direction (e.g. Franklin and Colombo 1978)."[76]

"A delay-Doppler image of Saturn's rings at a frequency of 2380 MHz (12.6 cm) is compared to a model image constructed by reprojecting a pair of HST images taken at 439 nm. Time delay increases from bottom to top, and Doppler shift increases from left to right. The effective spatial resolution is 2000 km by 15000 km."[76]

Radios[edit | edit source]

In this simulated image of Saturn's rings, color is used to present information about ring particle sizes in different regions based on the measured attenuations of three radio signals. Credit: NASA / Jet Propulsion Lab.
Dragon Storm: photo was taken on September 15, 2004 by Cassini spacecraft. Credit: NASA/JPL/Space Science Institute.

"Three simultaneous radio signals at wavelengths of 0.94, 3.6, and 13 centimeters (Ka-, X-, and S-bands) were sent from Cassini through the rings to Earth. The observed change of each signal as Cassini moved behind the rings provided a profile of the distribution of ring material and an optical depth profile."[77]

"This simulated image was constructed from the measured optical depth profiles of the Cassini Division and ring A. It depicts the observed structure at about 10 kilometers (6 miles) in resolution. The image shows the same ring A region depicted in a similar image (Multiple Eyes of Cassini), using a different color scheme to enhance the view of a remarkable array of over 40 wavy features called 'density waves' uncovered in the May 3 radio occultation throughout ring A."[77]

"Color is used to represent information about ring particle sizes based on the measured effects of the three radio signals. Shades of red [purple] indicate regions where there is a lack of particles less than 5 centimeters (about 2 inches) in diameter. Green and blue shades indicate regions where there are particles of sizes smaller than 5 centimeters (2 inches) and 1 centimeter (less than one third of an inch), respectively."[77]

"Note the gradual increase in shades of green towards the outer edge of ring A. It indicates gradual increase in the abundance of 5-centimeter (2-inch) and smaller particles. Note also the blue shades in the vicinity of the Keeler gap (the narrow dark band near the edge of ring A). They indicate increased abundance of even smaller particles of diameter less than a centimeter. Frequent collisions between large ring particles in this dynamically active region likely fragment the larger particles into more numerous smaller ones."[77]

The image at left is Saturn's atmosphere and its rings shown "in a false color composite made from Cassini images taken in near infrared light through filters that sense different amounts of methane gas. Portions of the atmosphere with a large abundance of methane above the clouds are red, indicating clouds that are deep in the atmosphere. Grey indicates high clouds and brown indicates clouds at intermediate altitudes. The rings are bright blue because there is no methane gas between the ring particles and the camera."[78]

"A large, bright and complex convective storm that appeared in Saturn's southern hemisphere in mid-September 2004 was the key in solving a long-standing mystery about the ringed planet."[78]

"The complex feature with arms and secondary extensions just above and to the right of center is called the Dragon Storm. It lies in a region of the southern hemisphere referred to as "storm alley" by imaging scientists because of the high level of storm activity observed there by Cassini in the last year."[78]

Plasma objects[edit | edit source]

Astronomers using the NASA/ESA Hubble Space Telescope have captured new images of the dancing auroral lights at Saturn’s north pole. Credit: NASA, ESA Acknowledgement: J. Nichols (University of Leicester).
Auroras on Saturn can shine for days. Credit: NASA/ESA/STScI/A. Schaller.

Astronomers using the NASA/ESA Hubble Space Telescope have captured new images of the dancing auroral lights at Saturn’s north pole shown in the images above.

"The ultraviolet images were taken by Hubble’s Advanced Camera for Surveys during April and May of last year from the space telescope’s perspective in orbit around Earth. The images are able to provide the first detailed look at dynamics in the “choreography” of auroral glow because Hubble captured them right at that very moment when Saturn’s magnetic field is blasted by particles streaming from the sun."[50]

"Hubble managed to capture a particularly dynamic light show: Some bursts of light shooting around the polar regions traveled at least three times faster than the speed of Saturn’s rotation. (The planet has a 10-hour rotation period.)"[50]

"Saturn's corona plays a major role in supplying hydrogen to the circumplanetary volume."[79]

"This cloud probably connects to the extended hydrogen corona of Saturn (Broadfoot et al., 1981; Shemansky and Hall, 1992) and to hydrogen-rich icy surfaces in the inner magnetosphere."[80]

Saturn's auroras are "magnificently tall, rising hundreds of miles above the planet’s poles. And unlike on Earth where bright displays fizzle after only a few hours, auroras on Saturn can shine for days."[81]

Gaseous objects[edit | edit source]

Saturn is a gas giant.

Atmospheres[edit | edit source]

"Light rays here travel a much longer path through the relatively cloud-free upper atmosphere. Along this path, shorter wavelength blue light rays are scattered effectively by gases in the atmosphere, and it is this scattered light that gives the region its blue appearance. Why the upper atmosphere in the northern hemisphere is so cloud-free is not known, but may be related to colder temperatures brought on by the ring shadows cast there."[55]

"Shadows cast by the rings surround the pole, looking almost like dark atmospheric bands. The ring shadows at higher latitudes correspond to locations on the ringplane that are farther from the planet--in other words, the northernmost ring shadow in this view is made by the outer edge of the A ring."[55]

"Spots of bright clouds also are visible throughout the region. This view is similar to an infrared image obtained by Cassini at nearly the same time (see PIA06567). The infrared view shows a great deal more detail in the planet's atmosphere, however."[55]

"Saturn's northern hemisphere is presently relatively cloud-free, and rays of sunlight take a long path through the atmosphere. This results in sunlight being scattered at shorter (bluer) wavelengths, thus giving the northernmost latitudes their bluish appearance at visible wavelengths."[56]

Prehistory[edit | edit source]

The prehistory period dates from around 7 x 106 b2k to about 7,000 b2k.

Saturn has been known since prehistoric times.[82]

Mesolithic[edit | edit source]

The mesolithic period dates from around 13,000 to 8,500 b2k.

"All that we have considered up to now indicates that Saturn [Arka] once exploded in a nova-like burst of light. The date of this event I would be hard-put to specify, even approximately, but possibly it took place about ten thousand years ago. The solar system and reaches beyond it were illuminated by the exploded star, and in a matter of a week the Earth was enveloped in waters of Saturnian origin."[83]

Ancient history[edit | edit source]

The ancient history period dates from around 8,000 to 3,000 b2k.

Apparently 5102 b2k (before the year 2000.0), -3102 or 3102 BC, is the historical year assigned to a Hindu table of planets that does include the classical planet Saturn.[84] "Babylonian astronomy, too, had a four-planet system. In ancient prayers the planets Saturn, Jupiter, Mars, and Mercury are invoked; ... and one speaks of "the four-planet system of the ancient astronomers of Babylonia."[85]"[86]

Babylonian astronomers systematically observed and recorded the movements of Saturn.[87]

Ancient Chinese and Japanese culture designated the planet Saturn as the earth star.

In ancient Hebrew, Saturn is called 'Shabbathai'.[88] Its angel is Cassiel. Its intelligence or beneficial spirit is Agiel (layga) and its spirit (darker aspect) is Zazel (lzaz).

In Ottoman Turkish, Urdu and Malay, its name is 'Zuhal'.

Anu[edit | edit source]

Anu may be an early Sumerian, Akkadian, and Babylonian name for Saturn.

"An, the oldest and highest of the Sumero-Babylonian gods, whose primordial age was "the year of abundance," signified Saturn, according to Jensen.6"[89]

Baal-hamon[edit | edit source]

The potential cruelty of Saturn was enhanced by his identification with Cronus, known for devouring his own children. He was thus equated with the Carthaginian god Ba'al Hammon, to whom children were supposedly sacrificed. Saturn was also among the gods the Romans equated with Yahweh, whose Sabbath (on Saturday) he shared as his holy day.

Modern scholars identify [Baal-hamon] variously with the Northwest Semitic god El or with Dagon.[90]

Ancient Greek writers identified him with the Titan Cronus. In ancient Rome, he was identified with Saturn.

Brahma[edit | edit source]

The Hindu Brahma, Yama, Vishnu, and Manu converge as representatives of a solitary supreme god and creator governing a lost paradise as the first king, setting forth the first moral codes, and imparting to mankind the fundamentals of civilization.

Cronus[edit | edit source]

The Greeks had made the outermost planet sacred to Cronus,[91] and the Romans followed suit.

El[edit | edit source]

In the Canaanite religion, or Levantine religion as a whole, Ēl or Il was the supreme god, the father of humankind and all creatures and the husband of the goddess Asherah as recorded in the clay tablets of Ugarit ... The noun ʾēl was found at the top of a list of gods as the "Ancient of gods" or the "Father of all gods", in the ruins of the royal archive of the Ebla civilization, in the archaeological site of Tell Mardikh in Syria dated to 2300 BC.

Ēl (rendered Elus or called by his standard Greek counterpart Cronus) is not the creator god or first god. Ēl is rather the son of Sky and Earth.

Joseph Fontenrose first demonstrated that, whatever their deep origins, at Ugarit Dagon was identified with El,[92]

Osiris[edit | edit source]

The gods Osiris, Anubis, and Horus are shown from a tomb painting. Credit: A. Parrot.
This is a detail of a frieze on a wall of tomb QV66, the burial place of Nefertari (c. 1295-1255 B.C.), royal wife of Ramesses the Great, featuring the Egyptian god Osiris. Credit: Mrgoodgame.

Osiris is the mythological father of the god Horus, whose conception is described in the Osiris myth, a central myth in ancient Egyptian belief. The myth described Osiris as having been killed by his brother Seth, who wanted Osiris' throne. Isis joined the fragmented pieces of Osiris, but the only body part missing was the phallus. Isis fashioned a golden phallus, and briefly brought Osiris back to life by use of a spell that she learned from [Geb] her father. This spell gave her time to become pregnant by Osiris before he again died. Isis later gave birth to Horus. As such, since Horus was born after Osiris' resurrection, Horus became thought of as a representation of new beginnings and the vanquisher of the evil Set.

"The Phoenician El - Saturn - has four eyes, as does the Orphic Kronos (Saturn)."[89]

"The Chinese Yellow Emperor Huang-ti--identified as Saturn--is also four-eyed.74"[89]

"Osiris, as the Ram of Mendes, is the god of "four faces on one neck."62"[89]

Have observers recorded images of sky entities in the green?

Romulus[edit | edit source]

Def. in Roman mythology, "[t]he legendary founder of Rome and the twin brother of Remus"[93] is called Romulus.

"Ioannes the Lydian, writing in the sixth century on the usage of his native town, says: 'Our own Philadelpheia still preserves a trace of the ancient belief. On the first day of the month (sc. January) there goes in procession no less a personage than Ianus himself, dressed up in a two-faced mask, and people call him Saturnus, identifying him with Kronos2.'"[94]

"The twins [Romulus and Remus], as in the case of Janus, attach themselves to the Universal Monarch as his two faces, looking in opposite directions."[89]

Saturnus[edit | edit source]

In ancient Roman mythology, the god Saturnus, from which the planet takes its name, was the god of agriculture.[95] The Romans considered Saturnus the equivalent of the Greek god Cronus.[95]

The Latins considered Saturn the predecessor of Jupiter. Saturn reigned in Latium during a mythical Golden Age reenacted every year at the festival of Saturnalia. Saturn also retained primacy in matters of agriculture and money. Unlike the Greek tradition of Cronus and Zeus, the usurpation of Saturn as king of the gods by Jupiter was not viewed by the Latins as violent or hostile; Saturn continued to be revered in his temple at the foot of the Capitol Hill, which maintained the alternative name Saturnius into the time of Varro.[96]

God[edit | edit source]

This is an image of a painting by artist Giorgio Vasari (1511–1574). Credit: Dodo Vasari.

"There is one God, greatest among gods and men, neither in shape nor in thought like unto mortals ... He abides ever in the same place motionless, and it befits him not to wander hither and thither."[97]

"Saturn, the old man who lives at the north pole, and brings with him to the children of men a sprig of evergreen (the Christmas tree), is familiar to the little folks under the name Santa Claus, for he brings each winter the gift of a new year."[98]

"The religions of all ancient nations ... associate the abode of the supreme God with the North Pole, the centre of heaven; or with the celestial space immediately surrounding it."[99]

"Lenormant, speaking of Rome and Olympia, remarks, "It is impossible not to note that the Capitoline was first of all the Mount of Saturn, and that the Roman archaeologists established a complete affinity between the Capitoline and Mount Cronios in Olympia, from the standpoint of their traditions and religious origin (Dionysius Halicarn., i., 34). This Mount Cronios is, as it were, the Omphalos of the sacred city of Elis, the primitive centre of its worship. It sometimes receives the name Olympos."1 Here is not only symbolism in general, but also a symbolism pointing to the Arctic Eden, already shown to be the primeval mount of Kronos, the Omphalos of the whole earth.2"[99]

"As an offshoot of these Hellenistic speculations we should place Tacitus, Histories V,2: "Iudaeos Creta insula profugos novissima Libyae insedisse memorant, qua tempestate Saturnus vi Jovis pulsus cesserit regnis" (quoted from Loeb Classical Library)."[100] i.e., "Jews were fugitives from the island of Crete and settled in Libya recorded the time when Saturn was driven from his throne by force of Jupiter".[100]

"The motif of Saturn handing over power to Jupiter derives, of course, from Hesiod's account of the succession of the gods in his Theogony, and his story of the five successive ages of men -- the first, or golden, age being under the reign of Kronos (Saturn) and the following ages being under the reign of Zeus (Jupiter) -- in his Works and Days (110ff.). These stories were often retold. Ovid, for example, combines in his Metamorphoses the stories in the Theogony and Works and Days, telling us how, "when Saturn was consigned to the darkness of Tartarus, and the world passed under the rule of Jove, the age of silver replaced that of gold."8"[101]

The image on the right is a painting by artist Giorgio Vasari (1511–1574). The main focus is on Cronus (Saturn) castrating Uranus (the Greek sky god). As both Uranus and Cronus are represented by men, this suggests that they were similar in nature.

Early history[edit | edit source]

A Statue of Krishna in the Sri Mariamman Temple, Singapore has Krishna shown with a flute. Credit: AngMoKio.

The early history period dates from around 3,000 to 2,000 b2k.

"Krishna ... is the [Daśāvatāra] eighth [avatar] incarnation of Lord Vishnu in Hinduism. ... Worship of the deity Krishna, either in the form of Vasudeva, Bala Krishna or Gopala can be traced to as early as 4th century BC.[102][103] He is often shown wearing a yellow silk dhoti and a peacock feather crown. The Harivamsa describes intricate relationships between Krishna Vasudeva, Sankarsana, Pradyumna and Aniruddha that would later form a Vaishnava concept of primary quadrupled expansion, or avatar.[104]

"The Hindu Atharva Veda speaks of the "four heavenly directions, having the wind as lord, upon which the sun looks out."63 This, of course, can only be the central sun, who is Brahma, a god of four faces. The myths also attribute four faces to Shiva.64 The central sun Prajapati takes the form of the four-eyed, four-faced, and four-armed Vivvakarman, the "all maker".65 Agni, too, faces "in all directions,"66 as does Krishna.67 ... There can no longer be any doubt that the four-eyed or four-faced god is Saturn, for the sun-planet appears in Babylonian myth as Ea (Sumerian Enki)-a god of four eyes that "behold all things."73"[89]

Classical history[edit | edit source]

The classical history period dates from around 2,000 to 1,000 b2k.

Pliny the Elder published Naturalis Historia circa 77-79 AD (1923-1921 b2k).

"68. Cf. PL. [Pliny the Elder], II, 138-139; SERV. [Servius], ad VERG., Aen., I, 42; XI, 259. Les foudres de Saturne sont des foudres d'hiver, ce qui correspond á la date de sa fête et plus fondamentalement aux liens entre cette divinité et l'aspect de [...] crise [...] de l'année que représente cette saison."[105] on page 151. This footnote may translate from the French to read: The thunderbolts (lightning) of Saturn are winter thunderbolts which correspond to the date of his birthday and more fundamentally to the links between this deity and the appearance of the annual crisis that represents this season.

"Ptolemy observed an opposition of Saturn A. D. 127 [1873 b2k], which was the basis for his determination of the elements of its orbit."[106]

Recent history[edit | edit source]

This painting of God the Father dates to ca. 1380 (620 b2k). Credit: Anonymous (France or Flanders).
God the Father is depicted with a dark halo. Credit: Anonymous (Swabia).
This is the frontispiece of Riccioli's 1651 New Almagest. Credit: G. B. Riccioli.
Here, God the Father has an apparent halo. Credit: Master of the Bonn Diptych.
Here, Michelangelo painted God in white with some green nearby. Credit: Michelangelo Buonarroti.
The page shows Huygens Systema Saturnium. Credit: Christiaan Huygens.
Here again, God the Father is painted in white. Credit: Ludovico Mazzolino.
This illustration included in Cellarius' book is a plate depicting the Earth-centered universe theorized by Claudius Ptolemy, the 2nd century A.D. geographer who lived in Alexandria, Egypt. Credit: Andreas Cellarius.
God the Father has a whitish bald head partially surrounded with whitish hair. Credit: Guercino.
This is a chart of the solar system out to the orbit of the planet Saturn. Credit: Richard Cumberland, translated from Latin by John Maxwell.

The recent history period dates from around 1,000 b2k to present.

The Franco-Flemish painting on the right has God the Father with a halo, dated to circa 1380 (620 b2k).

On the left is the frontispiece "of Riccioli's 1651 New Almagest. [In it mythological] figures observe the heavens with a telescope and weigh the heliocentric theory of Copernicus in a balance against his modified version of Tycho Brahe's geo-heliocentric system, in which the Sun, Moon, Jupiter and Saturn orbit the Earth while Mercury, Venus, and Mars orbit the Sun. The old Ptolemaic geocentric theory lies discarded on the ground, made obsolete by the telescope's discoveries. These are illustrated at top and include phases of Venus and Mercury and a surface feature on Mars (left), moons of Jupiter, rings of Saturn, and features on the moon (right). The balance tips in favor of Riccioli's "Tychonic" system."[107]

In the second image down on the right, God the Father has a dark halo. Dated circa 4th quarter of the 15th century (1475-1500, 525-500 b2k).

The third image down on the right is dated circa 1480-1490 (520-510 b2k) with God the Father having an apparent halo in white.

The second figure on the left contains Huygens Systema Saturnium. The top diagram shows how Saturn's appearance to us changes due the changing positions of the Earth (E) and Saturn as they orbit the Sun (G). The bottom portion contains Huygens observation of Saturn presenting its rings to us at their greatest inclination. Both parts date from 1659, 341 b2k.

In the fourth image down on the right, Michelangelo painted God in white with some green nearby, dated to 1508-1512 (492-588 b2k).

The fifth image down on the right has God the Father painted in white by Ludovico Mazzolino, dated to from 1510 until 1520 (490-480 b2k). The halo is gone but it appears a bald head replaces the disk of Saturn.

The third page down on the left is dated to 1661, 339 b2k, and describes the theory of Ptolemy.

The sixth image down on the right dated to circa 1635-1640 has God the Father with a whitish bald head partially surrounded with whitish hair.

The fourth page on the left is a chart of the Solar System up to the orbit of the planet Saturn. The tracks of three comets are indicated, which appeared in the years 1662, 1680 and 1682, respectively. The page is dated to 1727, 273 b2k.

Hypotheses[edit | edit source]

  1. If Saturn was a pole star for the Earth while in orbit around the Sun in recorded history, the astronomical observations of the time should record this in some way.

See also[edit | edit source]

References[edit | edit source]

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External links[edit | edit source]