Saturn

Saturn
Orbital characteristics (Epoch J2000)
Semi-major axis 1,426,725,413 km
9.537 070 32 AU
Orbital circumference 8.958 Tm
59.879 AU
Eccentricity 0.054 150 60
Perihelion 1,349,467,375 km
9.020 632 24 AU
Aphelion 1,503,983,449 km
10.053 508 40 AU
Orbital period 10,756.1995 d
(29.45 a)
Synodic period 378.10 d
Avg. orbital speed 9.639 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 the
ascending node
113.715 04°
Argument of the
perihelion
338.716 90°
Number of satellites 49 confirmed
Physical characteristics
Equatorial diameter 120,536 km [1]
(9.449 Earths)
Polar diameter 108,728 km
(8.552 Earths)
Oblateness 0.097 96
Surface area 4.27×1010 km2
(83.703 Earths)
Volume 7.46×1014 km3
(688.79 Earths)
Mass 5.6846×1026 kg
(95.162 Earths)
Mean density 0.6873 g/cm3
(less than water)
Equatorial gravity 8.96 m/s2
(0.914 gee)
Escape velocity 35.49 km/s
Rotation period 0.444 009 259 2 d
(10 h 39 min 22.400 00 s) 1
Rotation velocity 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 83.54°
Albedo 0.47
Avg. cloudtop temp. 93 K
Surface temp.
min mean max
82 K 143 K N/A K
Adjective Saturnian
Atmospheric characteristics
Atmospheric pressure 140 kPa
Hydrogen >93%
Helium >5%
Methane 0.2%
Water vapor 0.1%
Ammonia 0.01%
Ethane 0.0005%
Phosphine 0.0001%

Saturn is the sixth planet from the Sun. It is a gas giant, the second-largest planet in the solar system after Jupiter. Saturn has large rings consisting of mostly ice particles with a smaller amount of rocky debris. It was named after the Roman god Saturn. Its symbol is a stylized representation of the god's sickle (Unicode: ♄).

The Chinese, Korean, and Japanese cultures refer to the planet as the Earth Star, based on the Five Elements.

Physical characteristics

Saturn's shape is visibly flattened at the poles and bulging at the equator (an oblate spheroid); its equatorial and polar diameters vary 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 also the only one of the Solar System's planets less dense than water, with an average specific density of 0.69. This is only an average value, however; Saturn's upper atmosphere is less dense and its core is considerably more dense than water.

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 12000 K 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.


Saturn's temperature emissions, the prominent hot spot at the bottom of the image is right at Saturn's south pole

Saturn's atmosphere exhibits a banded pattern similar to Jupiter's, but Saturn's bands are much fainter and they're also much wider near the equator. Saturn's 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 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. Astronomers using infrared imaging have shown that Saturn has a warm polar vortex, and is the only planet in the solar system known to do so.

Rotational behavior

Since Saturn does not rotate on its axis at a uniform rate, two rotation periods have been assigned to it, like 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 in value 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). [2] The cause of the change is unknown.

Saturn's rings

Saturn is probably best known for its planetary rings, which make it one of the most visually remarkable objects in the solar system. See rings of Saturn for a list of the planet's rings.

History

The rings were first observed by Galileo Galilei in 1610 with his telescope, but he clearly did not know what to make of them. He wrote to the Grand Duke of Tuscany that "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.

The riddle of the rings was not solved until 1655 by Christiaan Huygens, using a telescope much more powerful than the ones available to Galileo in his time.

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.

Physical characteristics of the rings

The rings can be viewed using a quite modest modern telescope or with a good pair of binoculars. They extend from 6,630 km to 120,700 km above Saturn's equator, 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 that Saturn formed out of. 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, could be seen from Earth, the Voyagers 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 undiscovered, 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) and is thought to be a product of the disintegration of water ice from the rings into its components, oxygen and hydrogen. [3]

The dark side of the rings

Compare images from the Cassini spacecraft taken in March and October 2004, and a Pioneer 11 picture from 1979:

Cassini spacecraft: March 27, 2004; Frontlit rings. Notice both the shadow of Saturn on the rings, and the shadow of the rings onto the planet. The thick B ring is the brightest part of the ring system.
Pioneer 11 spacecraft: September 1, 1979; Backlit rings, showing the overall darkness of the rings from this angle. The thickest parts of the rings are almost invisible.
Cassini spacecraft: October 27, 2004; Backlit rings in detail. The thick B ring appears darkest from this side.

The side of Saturn's rings that is lit by the Sun looks very different to the backlit side, which is darker overall and appears almost black in the thick B ring. From Earth, we cannot appreciate this because the Earth cannot view Saturn from an angle that displays the backlit side of the rings, and our only views of it are from spacecraft. In 2004, the Cassini spacecraft revealed the first views of the backlit side in 25 years.

The spokes of the rings


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


Spokes imaged by Cassini in 2005.

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 behind the spokes is still unknown.

25 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.

Exploration of Saturn


A Hubble Space Telescope image, captured in October 1996 shows Saturn's rings from just past edge-on

Pioneer 11 flyby

Saturn was first visited by Pioneer 11 in 1979. It flew within 20,000 km of the planet's cloudtops. Low-resolution images were acquired of the planet and few of its moons. Resolution was not good enough to discern surface features, however. 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. It also measured the temperature of Titan. [4]

Voyager flybys

In November, 1980, Voyager 1 probe visited the Saturn system. It sent back the first high-resolution images of the planet, rings, and the 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 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 camera stuck 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.

Cassini orbiter

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. As of 2005, Cassini is conducting multiple flybys of Titan and icy satellites. The primary mission ends in 2008 when the spacecraft has completed 74 orbits around the planet.

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

Saturn's moons

Main article: Saturn's natural satellites

Saturn has a large number of moons, 49 are currently confirmed, 34 of which have names. The precise figure will never be certain 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. Saturn's most noteworthy moon is Titan, the only moon in the solar system to have a dense atmosphere.

Due to the tidal forces of Saturn, the moons are currently not at the same position as they were when they were first formed.

For a timeline of discovery dates, see Timeline of natural satellites.

Best viewing of Saturn


Saturn Oppositions: 2001-2029

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 favourable orientation of the rings relative to the Earth.


Saturn's Opposition Periods 2001-2005
Date of Opposition Distance
to Earth (AU)
Angular diameter
December 3, 2001 8.08 20.6 arcsec
December 17, 2002 8.05 20.7 arcsec
December 31, 2003 8.05 20.7 arcsec
January 13, 2005 8.08 20.6 arcsec

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 29 and a half years to make a complete circuit of the ecliptic against the background constellations of the zodiac. Optical aid (a large pair of binoculars or a telescope) magnifying at least 20X is required to clearly resolve Saturn's rings for most people.

Appearance

Stationary, retrograde Opposition Distance
to Earth (AU)
Maximum
Brightness (mag)
Diametre Inclination of ring Stationary, prograde Conjunction to Sun
October 26, 2003 December 31, 2003 8.05014 -0.5 20.70" -25,5° March 7, 2004 July 8, 2004
November 8, 2004 January 13, 2005 8.07564 -0.4 20.64" -22,8° March 22, 2005 July 23, 2005
November 22, 2005 January 27, 2006 8.12682 -0.2 20.51" -18,9° April 5, 2006 August 8, 2006
December 6, 2006 February 10, 2007 8.20033 0.0 20.32" -13,9° April 20, 2007 August 21, 2007
December 20, 2007 February 24, 2008 8.29136 0.2 20.10" -8,4° May 3, 2008 September 4, 2008
January 1, 2009 March 8, 2009 8.39440 0.5 19.85" -2,6° May 17, 2009 September 17, 2009
January 14, 2010 March 22, 2010 8.50379 0.5 19.60" 3,2° May 31, 2010 October 1, 2010
January 27, 2011 April 3, 2011 8.61392 0.4 19.35" 8,7° June 14, 2011 October 13, 2011
February 8, 2012 April 15, 2012 8.71959 0.2 19.11" 13,7° June 26, 2012 October 25, 2012
February 19, 2013 April 28, 2013 8.81618 0.1 18.90" 18,1° July 9, 2013 November 6, 2013
March 3, 2014 May 10, 2014 8.89968 0.1 18.73" 21,7° July 21, 2014 November 18, 2014
March 14, 2015 May 23, 2015 8.96672 0.0 18.59" 24,4° August 2, 2015 November 30, 2015
March 25, 2016 June 3, 2016 9.01492 0.0 18.49" 26° August 13, 2016 December 10, 2016
April 6, 2017 June 15, 2017 9.04268 0.0 18.43" 26,6° August 25, 2017 December 21, 2017
April 18, 2018 June 27, 2018 9.04884 0.0 18.42" 26° September 6, 2018 January 2, 2019
April 30, 2019 July 9, 2019 9.03285 0.1 18.45" 24,3° September 18, 2019 January 13, 2020
May 11, 2020 July 20, 2020 8.99474 0.1 18.53" 21,7° September 29, 2020 January 24, 2021

Saturn in fiction and film

Saturn is a popular setting for science fiction novels and films, although the planet tends to be used as a pretty backdrop rather than as an important part of the plot.

  • In H. P. Lovecraft's Cthulhu Mythos (1928–), Saturn was known as Cykranosh in the Hyperborean Era, both Tsathoggua and Atlach-Nacha came to Earth from there, and Tsathoggua's paternal uncle Hziulquoigmnzhah still resides there.
  • In Isaac Asimov's short story The Martian Way (1952), Martian colonists use a chunk of ice from Saturn's rings to bring water to the dry world.
  • Kurt Vonnegut's novel The Sirens of Titan (1959) is partly set on Titan, Saturn's best known moon.
  • In the Star Trek universe (1966–), Saturn is used for the Starfleet Academy Flight Range.
  • In Arthur C. Clarke's novel version of 2001: A Space Odyssey (1968), a spacecraft visits the Saturnian system. Clarke's later novel Imperial Earth (1976) takes place partially at a human colony on Titan.
  • Douglas Trumbull's film Silent Running (1972) features an ark-like spacecraft travelling through the Saturnian system.
  • The film Saturn 3 (1980) is mostly set on one of Saturn's moons, but also features a journey through the planet's rings.
  • The science fiction anime series The Super Dimension Fortress Macross (1982–1983) has one episode that takes place in Saturn's rings, and the beginning of the movie adaptation The Super Dimension Fortress Macross: Do You Remember Love? takes place near the moon Titan and Saturn's rings.
  • Tim Burton's film Beetlejuice (1988) is partly set on a fictional Saturn, populated by giant sandworms.
  • The Citadel research and mining space station, setting of the computer game System Shock (1994), is in orbit of Saturn for most of the game.
  • Stephen Baxter's novel Titan (1997) is focused on the moon Titan, but contains vivid depictions of a journey through the Saturnian system.
  • In Michael McCollum's novel The Clouds of Saturn (1998), SparrowHawk pilots Larson Sands and Halley Trevanon fight against the Northern Alliance during a time when the Sun has flared out of control and boiled Earth's oceans away.
  • In the sci-fi anime Cowboy Bebop (1998), in the year 2068 a war was fought on Titan.
  • Ben Bova's novel Saturn (2003) is about a spacecraft travelling toward the planet, although Saturn itself does not figure greatly in the story.
  • Warhammer 40,000's universe places the headquarters of the Grey Knights and Ordo Malleus in Saturn's moons, owing to their defensive capability.
  • In the sixth book of the Yoko Tsuno comic book series (Les 3 soleils de Vinéa), a small part of the action takes place on a Vinean space station in orbit around Saturn. Saturn's moon Titan is also briefly mentioned and depicted. Other Saturnian moons are visible but not named.

Saturn in various cultures

Chinese and Japanese culture designate the planet Saturn as "Earth Star." This is based on Five Elements which was 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.

Saturn from Cassini-Huygens, Michele Dougherty, Larry Esposito

See also

Saturn in astrology

Links



(moon navigator) | Saturn | Pan | ...



Saturn's natural satellites


Pan | Daphnis | Atlas | Prometheus | S/2004 S 6 | S/2004 S 4 | S/2004 S 3 | Pandora | Epimetheus and Janus | Mimas | Methone | Pallene | Enceladus | Telesto, Tethys, and Calypso | Polydeuces, Dione, and Helene | Rhea | Titan | Hyperion | Iapetus | Kiviuq | Ijiraq | Phoebe | Paaliaq | Skathi | Albiorix | S/2004 S 11 | Erriapo | Siarnaq | S/2004 S 13 | Tarvos | Mundilfari | S/2004 S 17 | Narvi | S/2004 S 15 | S/2004 S 10 | Suttungr | S/2004 S 12 | S/2004 S 18 | S/2004 S 9 | S/2004 S 14 | S/2004 S 7 | Thrymr | S/2004 S 16 | Ymir | S/2004 S 8

see also: Rings of Saturn | Cassini-Huygens | Themis



Our Solar System

Sun | Mercury | Venus | Earth (Moon) | Mars | Asteroid belt

Jupiter | Saturn | Uranus | Neptune | Pluto (Charon) | Kuiper belt | Scattered disc | Oort cloud

See also astronomical objects and the solar system's list of objects, sorted by radius or mass

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