Saturn

From Wikipedia, the free encyclopedia

Note: This article contains special characters.

Saturn  

Saturn, as seen by Cassini
Orbital characteristics
Epoch J2000
Aphelion distance:	1,503,983,449 km 10.053 508 40 AU 934,534,231 miles
Perihelion distance:	1,349,467,375 km 9.020 632 24 AU 838,522,163 miles
Semi-major axis:	1,426,725,413 km 9.537 070 32 AU 886,528,196 miles
Orbital circumference:	8.958 Tm 59.879 AU
Eccentricity:	0.054 150 60
Sidereal period:	10,756.1995 day (29.46 yr)
Synodic period:	378.10 day
Avg. orbital speed:	9.638 km/s
Max. orbital speed:	10.183 km/s
Min. orbital speed:	9.137 km/s
Inclination:	2.484 46° (5.51° to Sun's equator)
Longitude of ascending node:	113.71532811 04°
Argument of perihelion:	338.716 90°
Satellites:	56 confirmed[1]
Physical characteristics
Equatorial radius:	60,268 km[2] (9.4492 Earths)
Polar radius:	54,364 km (8.5521 Earths)
Oblateness:	0.097 96
Surface area:	4.27×1010 km² (83.703 Earths)
Volume:	8.27×1014 km³ (763 Earths)
Mass:	5.6846×1026 kg (95.152 Earths)
Mean density:	0.6873 g/cm³ (less than water)
Equatorial surface gravity:	8.96 m/s2 (0.914 g)
Escape velocity:	35.49 km/s
Sidereal rotation period:	0.449 375 day (10 h 47 min 6 s)[3]
Rotation velocity at equator:	9.87 km/s = 35,500 km/h (at the equator)
Axial tilt:	26.73°
Right ascension of North pole:	40.59° (2 h 42 min 21 s)
Declination of North pole:	83.54°
Albedo:	0.47
Surface temp.:    Surface    Cloudtop	min mean max 82 K 143 K N/A 93 K
Adjectives:	Saturnian
Atmosphere
Surface pressure:	140 kPa
Composition:	>93% hydrogen >5% helium 0.2% methane 0.1% water vapor 0.01% ammonia 0.0005% ethane 0.0001% phosphine

Saturn (IPA: [ˈsæɾɚn], [ˈsætən]) is the sixth planet from the Sun. It is a gas giant (also known as a Jovian planet, after the planet Jupiter), the second-largest planet in the Solar System after Jupiter. Saturn has a prominent system of rings, consisting mostly of ice particles with a smaller amount of rocky debris and dust. It was named after the Roman God Saturn (the Greek equivalent is Cronos, father of Zeus). Its symbol is a stylized representation of the god's sickle (Unicode: ♄).^[4][5]

[edit] Physical characteristics

Saturn's temperature emissions: The prominent hot spot at the bottom of the image is at Saturn's south pole.

Saturn is an oblate spheroid; that is, it is flattened at the poles and bulges at the equator. Its equatorial and polar diameters differ by almost 10% (120,536 km vs. 108,728 km). This is the result of its rapid rotation and fluid state. The other gas planets are also oblate, but to a lesser degree. Saturn is the only planet of the Solar System that is less dense than water. Although Saturn's core is considerably more dense than water, the average specific density of the planet is 0.69 g/cm³ due to the gaseous atmosphere.

Saturn's interior is similar to Jupiter's, having a rocky core at the center, a liquid metallic hydrogen layer above that, and a molecular hydrogen layer above that. Traces of various ices are also present. Saturn has a very hot interior, reaching 12,000 kelvins (11,700 °C) at the core, and it radiates more energy into space than it receives from the Sun. Most of the extra energy is generated by the Kelvin-Helmholtz mechanism (slow gravitational compression), but this alone may not be sufficient to explain Saturn's heat production. An additional proposed mechanism by which Saturn may generate some of its heat is the "raining out" of droplets of helium deep in Saturn's interior, the droplets of helium releasing heat by friction as they fall down through the lighter hydrogen.

Visual comparison of Saturn and Earth

Saturn's atmosphere exhibits a banded pattern similar to Jupiter's (in fact, the nomenclature is the same), but Saturn's bands are much fainter and are also much wider near the equator. Saturn's winds are among the Solar System's fastest. Voyager data indicates peak easterly winds of 500 m/s (1116 mph).^[6] Saturn's finer cloud patterns were not observed until the Voyager flybys. Since then, however, Earth-based telescopy has improved to the point where regular observations can be made.

Saturn's usually bland atmosphere occasionally exhibits long-lived ovals and other features common on Jupiter. In 1990 the Hubble Space Telescope observed an enormous white cloud near Saturn's equator which 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 Saturnian phenomenon with a roughly 30-year periodicity. 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.^[7]

In recent images from the Cassini spacecraft, Saturn's northern hemisphere appears a bright blue, similar to Uranus, as can be seen in the image above. This blue color cannot currently be observed from Earth, because Saturn's rings are currently blocking its northern hemisphere. The color is most likely caused by Rayleigh scattering.

North polar hexagonal cloud feature, discovered by Voyager 1 and confirmed in 2006 by Cassini. [1] [2]

Astronomers using infrared imaging have shown that Saturn has a warm polar vortex, and is the only such planet known in the solar system.

A persisting hexagonal wave pattern around the north polar vortex in the atmosphere at about 78°N was first noted in the Voyager images.^[8][9] Unlike the north pole, HST imaging of the south polar region indicates the presence of a jet stream, but no strong polar vortex nor any hexagonal standing wave.^[10] However, NASA reported in November 2006 that the Cassini spacecraft observed a 'hurricane-like' storm locked to the south pole that had a clearly defined eyewall.^[11] This observation is particularly notable because eyewall clouds have not been seen on any planet other than Earth (including a failure to observe an eyewall in the Great Red Spot of Jupiter by the Galileo spacecraft).^[12]

The straight sides of the northern polar hexagon are each about 13,800 kilometers long. The entire structure rotates with a period of 10h 39m 24s, the same period as that of the planet's radio emissions, which is assumed to be equal to the period of rotation of Saturn's interior. The hexagonal feature does not shift in longitude like the other clouds in the visible atmosphere.

The pattern's origin is a matter of much speculation. Most astronomers seem to favor some sort of standing-wave pattern in the atmosphere; but the hexagon might be a novel sort of aurora. More extreme speculation has Saturn's radio emissions emanating from the hexagon (something we can see and which has the right rotation period) rather than from the planet's interior (something we cannot see).^[13] Polygon shapes have been replicated in spinning buckets of fluid on laboratory scales.^[14]

[edit] Rotational behavior

Animated gif of hexagonal cloud feature.

Since Saturn does not rotate on its axis at a uniform rate, multiple rotation periods have been assigned to it (as in Jupiter's case): System I has a period of 10 h 14 min 00 s (844.3°/d) and encompasses the Equatorial Zone, which extends from the northern edge of the South Equatorial Belt to the southern edge of the North Equatorial Belt. All other Saturnian latitudes have been assigned a rotation period of 10 h 39 min 24 s (810.76°/d), which is System II. System III, based on radio emissions from the planet, has a period of 10 h 39 min 22.4 s (810.8°/d); because it is very close to System II, it has largely superseded it.

While approaching Saturn in 2004, the Cassini spacecraft found that the radio rotation period of Saturn had increased slightly, to approximately 10 h 45 m 45 s (± 36 s).^[15] The cause of the change is unknown — however, it is thought that this is due to a movement of the radio source to a different latitude inside Saturn, with a different rotational period, rather than an actual change in Saturn's rotation.

In March of 2007 it was reported that the variance in measured rotation periods may actually be caused by geyser activity on Saturn's moon Enceladus. The water vapor emitted into Saturnian orbit by this activity becomes charged and "weighs down" Saturn's magnetic field, slowing its rotation slightly relative to the rotation of the planet itself. If true, this means that there is no currently known method of determining the actual rotation rate of Saturn's core.^[16]

[edit] Planetary rings

The rings of Saturn, as imaged by Cassini in 2007

Main article: Rings of Saturn

Saturn is probably best known for its system of planetary rings, which makes it one of the most visually remarkable objects in the solar system.

[edit] History

The rings were first observed by Galileo Galilei in 1610 with his telescope, but he was unable to identify them as such. He wrote to the Duke of Tuscany that "The planet Saturn is not alone, but is composed of three, which almost touch one another and never move nor change with respect to one another. They are arranged in a line parallel to the zodiac, and the middle one (Saturn itself) is about three times the size of the lateral ones [the edges of the rings]." He also described Saturn as having "ears." In 1612 the plane of the rings was oriented directly at the Earth and the rings appeared to vanish, and then in 1613 they reappeared again, further confusing Galileo.^[17]

In 1655, Christiaan Huygens became the first person to suggest that Saturn was surrounded by a ring. Using a telescope that was far superior to those available to Galileo, Huygens observed Saturn and wrote that "It [Saturn] is surrounded by a thin, flat, ring, nowhere touching, inclined to the ecliptic."^[18]

In 1675, Giovanni Domenico Cassini determined that Saturn's ring was actually composed of multiple smaller rings with gaps between them; the largest of these gaps was later named the Cassini Division.

In 1859, James Clerk Maxwell demonstrated that the rings could not be solid or they would become unstable and break apart. He proposed that the rings must be composed of numerous small particles, all independently orbiting Saturn.^[19] Maxwell's theory was proven correct in 1895 through spectroscopic studies of the rings carried out by James Keeler of Lick Observatory.

[edit] Physical characteristics

The rings can be viewed using a quite modest modern telescope or with good binoculars. They extend from 6,630 km to 120,700 km above Saturn's equator, average close to one kilometer in thickness and are composed of silica rock, iron oxide, and ice particles ranging in size from specks of dust to the size of a small automobile. There are two main theories regarding the origin of Saturn's rings. One theory, originally proposed by Édouard Roche in the 19th century, is that the rings were once a moon of Saturn whose orbit decayed until it came close enough to be ripped apart by tidal forces (see Roche limit). A variation of this theory is that the moon disintegrated after being struck by a large comet or asteroid. The second theory is that the rings were never part of a moon, but are instead left over from the original nebular material from which Saturn formed. This theory is not widely accepted today, since Saturn's rings are thought to be unstable over periods of millions of years and therefore of relatively recent origin.

While the largest gaps in the rings, such as the Cassini Division and Encke Division, can be seen from Earth, the Voyager spacecrafts discovered the rings to have an intricate structure of thousands of thin gaps and ringlets. This structure is thought to arise from the gravitational pull of Saturn's many moons in several different ways. Some gaps are cleared out by the passage of tiny moonlets such as Pan, many more of which may yet be discovered, and some ringlets seem to be maintained by the gravitational effects of small shepherd satellites such as Prometheus and Pandora. Other gaps arise from resonances between the orbital period of particles in the gap and that of a more massive moon further out; Mimas maintains the Cassini division in this manner. Still more structure in the rings actually consists of spiral waves raised by the moons' periodic gravitational perturbations.

Data from the Cassini space probe indicates that the rings of Saturn possess their own atmosphere, independent of that of the planet itself. The atmosphere is composed of molecular oxygen gas (O₂) produced when ultraviolet light from the Sun disintegrates water ice in the rings. Chemical reactions between water molecule fragments and further ultraviolet stimulation create and eject, among other things O₂. According to models of this atmosphere, H₂ is also present. The O₂ and H₂ atmospheres are so sparse that if the entire atmosphere were somehow condensed onto the rings, it would be on the order of one atom thick.^[20] The rings also have a similarly sparse OH (hydroxide) atmosphere. Like the O₂, this atmosphere is produced by the disintegration of water molecules, though in this case the disintegration is done by energetic ions that bombard water molecules ejected by Saturn's moon Enceladus. This atmosphere, despite being extremely sparse, was detected from Earth by the Hubble Space Telescope.^[21]

Saturn shows complex patterns in its brightness. Most of the variability is due to the changing aspect of the rings, and this goes through two cycles every orbit. However, superimposed on this is variability due to the eccentricity of the planet's orbit that causes the planet to display brighter oppositions in the northern hemisphere than it does in the southern (Henshaw, C., 2003).^[22]

In 1980 Voyager I made a fly-by of Saturn that showed the F-ring to be composed of three narrow rings that appeared to be braided in a complex structure; it is now known that the outer two rings consist of knobs, kinks and lumps that give the illusion of braiding, with the less bright third ring lying inside them.

[edit] Spokes of the rings

Spokes in the B ring, imaged by Voyager 2 in 1981

Until 1980, the structure of the rings of Saturn was explained exclusively as the action of gravitational forces. The Voyager spacecraft found radial features in the B ring, called spokes, which could not be explained in this manner, as their persistence and rotation around the rings were not consistent with orbital mechanics. The spokes appear dark against the lit side of the rings, and light when seen against the unlit side. It is assumed that they are connected to electromagnetic interactions, as they rotate almost synchronously with the magnetosphere of Saturn. However, the precise mechanism generating the spokes is still unknown.

Spokes imaged by Cassini in 2005

Twenty-five years later, Cassini observed the spokes again. They appear to be a seasonal phenomenon, disappearing in the Saturnian midwinter/midsummer and reappearing as Saturn comes closer to equinox. The spokes were not visible when Cassini arrived at Saturn in early 2004. Some scientists speculated that the spokes would not be visible again until 2007, based on models attempting to describe spoke formation. Nevertheless, the Cassini imaging team kept looking for spokes in images of the rings, and the spokes reappeared in images taken September 5, 2005.

[edit] Natural satellites

Four of Saturn's moons: Dione, Titan, Prometheus (edge of rings), Telesto (top center)

Main article: Saturn's natural satellites

Saturn has a large number of moons. The precise figure is uncertain, as the orbiting chunks of ice in Saturn's rings are all technically moons, and it is difficult to draw a distinction between a large ring particle and a tiny moon. As of 2006, a total of 56 individual moons have been identified, along with 3 unconfirmed moons that could be small dust clumps in the rings. Many of the moons are very small: out of 56, 30 are less than 10 km in diameter, and another 13 less than 50 km.^[23] Only seven of them are massive enough to have collapsed into spheroids under their own gravitation. These are compared with Earth's moon in the table below. Saturn's most noteworthy moon is Titan, the only moon in the solar system to have a dense atmosphere.

Saturn's rings cut across an eerie scene that is ruled by Titan's luminous crescent and globe-encircling haze, broken by the small moon Enceladus, whose cryovolcanos are dimly visible at its south pole. North is up.

Traditionally, most of Saturn's other moons are named after actual Titans of Greek mythology. This started because John Herschel — son of William Herschel, discoverer of Mimas and Enceladus — suggested doing so in his 1847 publication Results of Astronomical Observations made at the Cape of Good Hope,[2] because they were the sisters and brothers of Cronos (the Greek Saturn).

For a timeline of discovery dates, see Timeline of discovery of Solar System planets and their natural satellites.

[edit] Exploration of Saturn

A Hubble Space Telescope image, captured in October 1996, shows Saturn's rings from just past edge-on. Credit: NASA/ESA.

[edit] Pioneer 11 flyby

Saturn was first visited by Pioneer 11 in September 1979. It flew within 20,000 km of the planet's cloud tops. Low-resolution images were acquired of the planet and a few of its moons; the resolution of the images was not good enough to discern surface features. The spacecraft also studied the rings; among the discoveries were the thin F-ring and the fact that dark gaps in the rings are bright when viewed towards the Sun, or in other words, they are not empty of material. Pioneer 11 also measured the temperature of Titan.^[24]

[edit] Voyager flybys

In November 1980, the Voyager 1 probe visited the Saturn system. It sent back the first high-resolution images of the planet, rings, and satellites. Surface features of various moons were seen for the first time. Voyager 1 performed a close flyby of Titan, greatly increasing our knowledge of the atmosphere of the moon. However, it also proved that Titan's atmosphere is impenetrable in visible wavelengths, so no surface details were seen. The flyby also changed the spacecraft's trajectory out from the plane of the solar system.

Almost a year later, in August 1981, Voyager 2 continued the study of the Saturn system. More close-up images of Saturn's moons were acquired, as well as evidence of changes in the atmosphere and the rings. Unfortunately, during the flyby, the probe's turnable camera platform stuck for a couple of days and some planned imaging was lost. Saturn's gravity was used to direct the spacecraft's trajectory towards Uranus.

The probes discovered and confirmed several new satellites orbiting near or within the planet's rings. They also discovered the small Maxwell and Keeler gaps.

[edit] Cassini orbiter

Saturn eclipses the sun, as seen from Cassini.

On July 1, 2004, the Cassini-Huygens spacecraft performed the SOI (Saturn Orbit Insertion) maneuver and entered into orbit around Saturn. Before the SOI, Cassini had already studied the system extensively. In June 2004, it had conducted a close flyby of Phoebe, sending back high-resolution images and data.

The orbiter completed two Titan flybys before releasing the Huygens probe on December 25, 2004. Huygens descended onto the surface of Titan on January 14, 2005, sending a flood of data during the atmospheric descent and after the landing. During 2005 Cassini conducted multiple flybys of Titan and icy satellites.

On March 10, 2006, NASA reported that the Cassini probe found evidence of liquid water reservoirs that erupt in geysers on Saturn's moon Enceladus.^[25]

On September 20, 2006, a Cassini probe photograph revealed a previously undiscovered planetary ring, outside the brighter main rings of Saturn and inside the G and E rings.^[26]

In July 2006, Cassini saw the first proof of hydrocarbon lakes near Titan's north pole, which was confirmed in January 2007. In March 2007, additional images near Titan's north pole discovered hydrocarbon "seas", the largest of which is almost the size of the Caspian Sea.^[27]

As of 2006 the probe has discovered and confirmed 4 new satellites. Its primary mission will end in 2008 when the spacecraft will be expected to have completed 74 orbits around the planet.

For the latest information and news releases, see Cassini website.

Picture of a large hurricane-like storm on the south pole of Saturn

[edit] Best viewing of Saturn

Saturn Oppositions: 2001-2029

Saturn has been known since prehistoric times. It is the most distant of the five planets easily visible to the naked eye, the other four being Mercury, Venus, Mars, and Jupiter (Uranus is visible to the naked eye in very dark skies), and was the last planet known to early astronomers until Uranus was discovered in 1781. Saturn appears to the naked eye in the night sky as a bright, yellowish star varying usually between magnitude +1 and 0 and takes approximately 29½ years to make a complete circuit of the ecliptic against the background constellations of the zodiac. Optical aid (large binoculars or a telescope) magnifying at least 20X is required to clearly resolve Saturn's rings for most people.

While it is a rewarding target for observation for most of the time it is visible in the sky, Saturn and its rings are best seen when the planet is at or near opposition (the configuration of a planet when it is at an elongation of 180° and thus appears opposite the Sun in the sky). In the opposition on January 13, 2005, Saturn appeared at its brightest until 2031, mostly due to a favorable orientation of the rings relative to the Earth.

[edit] Saturn in various cultures

In Hindu astrology, there are nine planets, known as Navagrahas. Saturn is known as "Sani" or "Shani", the Judge among all the planets, and determines everyone according to their own performed deeds bad or good.

Chinese and Japanese culture designate the planet Saturn as the earth star (土星). This is based on Five Elements which were traditionally used to classify natural elements.

In Hebrew, Saturn is called 'Shabbathai'. Its Angel is Cassiel. Its Intelligence, or beneficial spirit, is Agiel (layga), and its spirit (darker aspect) is Zazel (lzaz). See: Kabbalah.

In Ottoman Turkish and in Malay, its name is 'Zuhal', derived from Arabic زحل.

Saturn was also called Φαίνων, Phainon ("shiner") by the Greeks.

[edit] See also

• Saturn in astrology
• Saturn in fiction
• Dragon Storm (astronomy)

[edit] References

• H. Karttunen, P. Kröger, et al., Fundamental Astronomy, Springer, 3th Ed., Helsinki, 2000.

[edit] External links

Wikimedia Commons has media related to:

Saturn (planet)

• Saturn at ESA/Hubble
• Saturn - About Space
• NASA's Saturn fact sheet
• NASA's Cassini mission to Saturn
• Change of seasons on Saturn
• Theoretical description of the rings of Saturn
• Saturn Research News
• A Trip Into Space Description and photos of Saturn
• Planets - Saturn A kid's guide to Saturn.
• A WAV file of radio emissions from Saturn
• NASA's Cassini Images of Hexagon on Saturn

v • d • e The Solar System
The Sun · Mercury · Venus · Earth · Mars · Ceres · Jupiter · Saturn · Uranus · Neptune · Pluto · Eris
Planets · Dwarf planets · Moons: Terrestrial · Martian · Asteroidal · Jovian · Saturnian · Uranian · Neptunian · Plutonian · Eridian
Small bodies:   Meteoroids · Asteroids (Asteroid belt) · Centaurs · TNOs (Kuiper belt/Scattered disc) · Comets (Oort cloud)
See also astronomical objects, the solar system's list of objects, sorted by radius or mass, and the Astronomy Portal