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This article is about the planet. For other uses, seeSaturn (disambiguation).

Saturn♄
Pictured in natural color approachingequinox,photographed byCassiniin July 2008; the dot in the bottom left corner isTitan
Designations
Pronunciation/ˈsætərn/(audio speaker iconlisten)[1]
Named after
Saturn
AdjectivesSaturnian/səˈtɜːrniən/,[2]Cronian[3]/ Kronian[4]/ˈkroʊniən/[5]
Orbital characteristics[10]
EpochJ2000.0
Aphelion1,514.50 million km (10.1238 AU)
Perihelion1,352.55 million km (9.0412 AU)
1,433.53 million km (9.5826 AU)
Eccentricity0.0565
378.09 days
9.68 km/s (6.01 mi/s)
317.020°[7]
Inclination
113.665°
2032-Nov-29[9]
339.392°[7]
Knownsatellites145in totalmoonlets.[10]
Physical characteristics[10]
Mean radius
58,232 km (36,184 mi)[a]
  • 60,268 km (37,449 mi)[a]
  • 9.449Earths
Polarradius
  • 54,364 km (33,780 mi)[a]
  • 8.552 Earths
Flattening0.09796
Circumference
  • 4.27×1010km2(1.65×1010sq mi)[12][a]
  • 83.703 Earths
Volume
  • 8.2713×1014km3(1.9844×1014cu mi)[a]
  • 763.59 Earths
Mass
  • 5.6834×1026kg
  • 95.159 Earths
0.687g/cm3(0.0248lb/cu in)[b](less than water)
0.22[13]
35.5 km/s (22.1 mi/s)[a]
10 h 32 m 36 s
(synodic; solar day)[6]
10h33m38s+ 1m52s
− 1m19s [14][15]
Equatorial rotation velocity
9.87 km/s (6.13 mi/s; 35,500 km/h)[a]
26.73°(to orbit)
North poleright ascension
40.589°; 2h42m21s
North poledeclination
83.537°
Albedo
Surfacetemp. min mean max
1bar 134 K
0.1bar 88 K[19] 97 K[20] 151 K[19]
−0.55[18]to +1.17[18]
14.5″ to 20.1″ (excludes rings)
Atmosphere[10]
Surfacepressure
140 kPa[21]
59.5 km (37.0 mi)
Composition by volume
96.3%±2.4%hydrogen(H
2)
3.25%±2.4%helium(He)
0.45%±0.2%methane(CH
4)
0.0125%±0.0075%ammonia(NH
3)
0.0110%±0.0058%hydrogen deuteride(HD)
0.0007%±0.00015%ethane(C
2H
6)
Ices:

Saturnis the sixthplanetfrom theSunin theSolar System.

Saturn is one of the fourgas giantplanets in the Solar System, withJupiter,Uranus,andNeptune.It is the second largest planet in the Solar System (Jupiter is the largest).[22]

Saturn was named after theRoman godSaturn.He was the Roman equivalent of theGreek godKronos.[23]Saturn's symbol is ♄ which is the symbol of Saturnus'sickle.[24]

Inside Saturn is probably acoreofiron,nickel,siliconandoxygencompounds, surrounded by a deep layer ofmetallic hydrogen,then a layer ofliquidhydrogenand liquidheliumand finally, an outergaseouslayer.[25]

Saturn has 146 knownmoonsorbitingthe planet.[26]The largest moon isTitan.Titan is larger involumethan the planetMercury.It is the second-largest moon in the Solar System. The largest moon is a moon of Jupiter,Ganymede.There are also manyringsaround Saturn. These rings are made oficewith somerocksand dust. Some people think that that the rings were made by a moonimpactor other event. Saturn is about 1,433,000,000km(870,000,000mi) on average from the Sun. Saturn takes 29.4Earth yearsin order to complete a revolution around the Sun.[27]

Physical features[change|change source]

Saturn compared to Earth
Saturn compared with the size of theEarth
Pen sketch with several labelled rings
Drawing of Saturn byRobert Hookein 1666

Saturn is a squished sphere. This means that it is flattened at thepolesand wider around theequator.[28]The planet'sequatorialdiameteris 120,536 km (74,898 mi). Its polar diameter (the distance from the north pole to the south pole through the centre) is 108,728 km (67,560 mi). This is a 9% difference.[29]Saturn has a flattened shape because of its very fastrotation.It rotates once every 10.8 Earth hours.

Saturn is the only planet in the Solar System that is lessdensethanwater.Even though the planet'scoreis very dense, it has agaseousatmosphere.This makes its average density is 0.69 g/cm3.This means if Saturn could be placed in a large pool of water, it would float.[30]

Atmosphere[change|change source]

The outer part of Saturn's atmosphere is made up of about 96%hydrogen,3%helium,0.4%methaneand 0.01%ammonia.There are also someacetylene,ethaneandphosphine.[31]

The hexagonal cloud
The north polarhexagonalcloud first found byVoyager 1and later byCassini

Saturn'scloudsshow a banded pattern. This is like the cloud bands seen on Jupiter. Saturn's clouds are muchfainterand the bands are wider at the equator. Saturn's lowest cloud layer is made up of water ice. It is about 10 km (6 mi) thick.[31]Thetemperaturethere is quite low, at 250K(-10°F,-23°C). However, scientists do not all agree on this. The layer above is made up ofammonium hydrosulfideice. It is about 77 km (48 mi) thick. Above it is a layer of ammonia ice clouds which are 80 km (50 mi) thick.[31]The highest layer is made up of hydrogen and helium gases. It goes to between 200 km (124 mi) and 270 km (168 mi) above the water cloud tops.Aurorascan be seen in Saturn in themesosphere.[31]The temperature at Saturn's cloud tops is very low, at 98 K (-283 °F, -175 °C). The temperatures in the inner layers are much higher than the outside layers because of theheatmade by Saturn's inside.[32]Saturn'swindsare some of the fastest in the Solar System. They can reach 1,800km/h(1,118mph),[33]ten times faster than winds onEarth.[34]

Storms and spots[change|change source]

Saturn's atmosphere can make oval shaped clouds. They are like the clearer spots seen on Jupiter. These oval spots are cyclonic storms, similar tocyclonesseen on Earth. In 1990, theHubble Space Telescopefound a very large white cloud near Saturn's equator. Storms like this one in 1990 were known asGreat White Spots.These unique storms only exist for a short time and only occur in about every 30 Earth years, in summersolstices in theNorthern Hemisphere.[35]Great White Spots were also found in 1876, 1903, 1933, and 1960.

TheVoyager 1spacecraft found ahexagonalcloudpatternnear Saturn's north pole at about78°N.TheCassini−Huygensprobe laterconfirmedit in 2006. Unlike the north pole, the south pole does not show any hexagonal clouds. The probe also found ahurricane-like storm on the south pole that showed aneyewall.Until this finding, eyewalls had only been seen on Earth.[36]

Interior[change|change source]

Saturn's inside is similar to Jupiter's inside. It has a small rocky core about the size of the Earth at itscenter.[28]It is very hot. Itstemperaturereaches 15,000K(26,540 °F (14,727 °C)). Saturn is so hot that it gives out moreheat energyinto space than it gets from theSun.[32]Above it is a thicker layer of metallic hydrogen, about 30,000 km (18,641 mi) deep. Above that layer is a region of liquid hydrogen and helium.[37]The core is heavy, with about 9 to 22 times more mass than the Earth's core.[38]

Magnetic field[change|change source]

Saturn has a naturalmagnetic fieldthat is weaker than Jupiter's. Like the Earth's, Saturn's field is a magneticdipole(it has a North and a South). Saturn's field is unique in that it is perfectlysymmetrical,unlike any other known planet.[39]This means the field is exactly in line with the planet'saxis.[39]Saturn generatesradio waves,but they are too weak to be detected from Earth.[40]The moon Titan orbits in the outer part of Saturn's magnetic field and gives outplasmato the field from theionisedparticlesin Titan's atmosphere.[41]

Rotation and orbit[change|change source]

Saturn's averagedistancefrom the Sun is over 1,400,000,000 km (886,000,000 mi). This is about nine times the distance from the Earth to the Sun. It takes 10,756 days, or about 29.4 years, for Saturn to orbit around the Sun.[42]This is known as Saturn'sorbital period.

Voyager 1measuredSaturn's rotation as being 10 hours, 14 minutes at the equator, 10 hours, 40 minutes closer to the poles, and 10 hours, 39 minutes, 24 seconds for the planet's inside.[43]This is known as itsrotational period.

Cassini measured the rotation of Saturn as being 10 hours, 45 minutes, 45 seconds ± 36 seconds.[44]That is about six minutes longer than the radio rotational period measured by the Voyager 1 and Voyager 2spacecrafts,which flew by Saturn in 1980 and 1981.

Saturn's rotational period is calculated by the rotation speed of radio waves given off by the planet. The Cassini−Huygens spacecraft found that the radio waves slowed down. This suggested that the rotational periodincreased.[44]Since scientists do not think Saturn's rotation is actually slowing down, the explanation may be that the magnetic field causes the radio waves.[44]

Planetary rings[change|change source]

See the main article:Rings of Saturn

Saturn is best known for itsplanetary ringswhich are easy to see with atelescope.There are seven named rings: A, B, C, D, E, F, and G.[45]They were named in the order they were found, which is different to their order from the planet. From the planet the rings are ordered: D, C, B, A, F, G and E.[45]: 57 

Some scientists think that the rings arematerialleft after a moon broke apart.[45]: 60 A new idea says that it was a very large moon, most of which crashed into the planet. This left a large amount of ice to form the rings and some of the moons. This includesEnceladus,which is thought to be made of ice.[45]: 61 

History[change|change source]

The rings were first found byGalileo Galileiin 1610, using his telescope. They did not look like rings to Galileo. He called them "handles". He thought that Saturn was three different planets that were right next to each other. In 1612, when the rings were facing edge on with the Earth, the rings disappeared, then reappeared again in 1613, further confusing Galileo.[46]In 1655,Christiaan Huygenswas the first person to say that Saturn was surrounded by rings. Using a much more powerful telescope than Galilei's, he said that Saturn "is surrounded by a thin, flat, ring, nowhere touching...".[46]In 1675,Giovanni Domenico Cassinifound that the planet's rings were in fact made of smaller rings with gaps. The largest ring gap was later named theCassini Division.In 1859,James Clerk Maxwellshowed that the rings cannot be solid, but are made of small particles, each orbiting Saturn on their own. Otherwise, it would become unstable or break apart.[47]James Keelerstudied the rings using aspectroscopein 1895 which proved Maxwell's theory.[48]

Physical features[change|change source]

The rings range from 6,630 km (4,120 mi) to 120,700 km (75,000 mi) above the planet's equator. While the equatorial circumference of Saturn is 378,675 km (235,298 miles). As proved by Maxwell, even though the rings appear to be solid and unbroken when viewed from above, the rings are made of small particles of rock and ice. They are only about 10 m (33 ft) thick; made ofsilicarock,iron oxideand ice particles.[45]: 55 The smallest particles are only specks of dust while the largest are the size of a house. The C and D rings also seem to have a "wave" in them, like waves in water.[45]: 58 These large waves are 500 m (1,640 ft) high, but only moving slowly at about 250 m (820 ft) each day.[45]: 58 Some scientists believe that the wave is caused by Saturn's moons.[49]Another idea is the waves were made by acomethitting Saturn in 1983 or 1984.[45]: 60 

The largest gaps in the rings are the Cassini Division and theEncke Division,both visible from theEarth.The Cassini Division is the largest, measuring 4,800 km (2,983 mi) wide.[50]However, when the Voyager spacecrafts visited Saturn in 1980, they discovered that the rings are a complex structure, made out of thousands of thin gaps and ringlets. Scientists believe this is caused by thegravitational forceof some of Saturn's moons. The tiny moonPanorbits inside Saturn's rings, creating a gap within the rings. Other ringlets keep their structure due to the gravitational force ofshepherd satellites,such asPrometheusandPandora.Other gaps form due to the gravitational force of a large moon farther away. The moonMimasis responsible for clearing away the Cassini gap.[50]

Recent data from the Cassini spacecraft has shown that the rings have their own atmosphere, free from the planet's atmosphere. The rings' atmosphere is made of oxygen gas, and it is produced when the Sun'sultravioletlight breaks up the water ice in the rings.Chemical reactionsalso occur between the ultraviolet light and the watermolecules,creating hydrogen gas. The oxygen and hydrogen atmospheres around the rings are very widely spaced.[51]As well as oxygen and hydrogen gas, the rings have a thin atmosphere made ofhydroxide(a combination of oxygen and hydrogen called an anion), which was discovered by the Hubble Space Telescope.[52]

Spokes[change|change source]

The spokes in Saturn's rings
The spokes in Saturn's rings, photographed by Voyager 2

The Voyager space probe discovered features shaped likerays,called spokes.[53]These were also seen later by the Hubble telescope. The Cassini probephotographedthe spokes in 2005.[53]They appear dark when lit by sunlight, and appear light against the unlit side of the planet. At first it was thought the spokes were made of microscopic dust particles, but new evidence shows that they are made of ice.[54] They rotate at the same rate as the planet'smagnetosphere,therefore, it is believed that they have a connection withelectromagnetism.However, what causes the spokes to form is still unknown. They appear to beseasonal,disappearing duringsolsticeand appearing again duringequinox.[55]

Moons[change|change source]

Saturn has a total of 146 moons;53 are named moons,and another 29 are still being studied.[56]Many of the moons are very small: 33 are less than 10 km (6 mi) in diameter and 13 moons are less than 50 km (31 mi).[57]Seven moons are large enough to be a near perfectspherecaused by their owngravity.These moons areTitan,Rhea,Iapetus,Dione,Tethys,Enceladusand Mimas.[58]Titan is the largest moon, larger than the planet Mercury, and it is the only moon in the Solar System to have a thick, dense atmosphere.[59][60]HyperionandPhoebeare the next largest moons, larger than 200 km (124 mi) in diameter.

Between December 2004 and January 2005 a man-made satellite called the Cassini−Huygens probe took lots of close photos of Titan. One part of this satellite, known as the Huygens probe, landed on Titan, on land. Named after the Dutch astronomer Christiaan Huygens, it was the first spacecraft to land in the outer Solar System.[61]The probe was designed to float in case it landed in liquid.[61]Its batteries lasted about 3 hours. Enceladus, the sixth largest moon, is about 500 km (311 mi) in diameter. It is one of the few outer solar system objects that showsvolcanicactivity.[62]In 2011, scientists discovered an electric link between Saturn and Enceladus. This is caused byionisedparticles from volcanos on the small moon interacting with Saturn's magnetic fields.[62]Similar interactions cause thenorthern lightson Earth.[63]

Exploration[change|change source]

Saturn from Cassini orbiter
Saturn as seen from the Cassini spacecraft in 2007

Saturn was first explored by thePioneer 11spacecraft in September 1979. It flew as close as 20,000 km (12,427 mi) above the planet's cloud tops. It took photographs of the planet and a few of its moons, but were low inresolution.It discovered a new, thin ring called the F ring. It also discovered that the dark ring gaps appear bright when viewed towards theSun,which shows the gaps are not empty. The spacecraft measured the temperature of the moon Titan.[64]

In November 1980, Voyager 1 visited Saturn and took higher resolution photographs of the planet, rings, and moons. These photos showed some of the surface features of the moons. Voyager 1 went close to Titan and gained much information about its atmosphere. In August 1981,Voyager 2continued to study the planet. Photos taken by the space probe showed that changes were happening to the rings and atmosphere. The Voyager spacecraft discovered a number of moons orbiting close to Saturn's rings, as well as discovering new ring gaps.

Drawing of Cassini in orbit around Saturn

On July 1, 2004, the Cassini−Huygens probe entered into orbit around Saturn. Before then, it flew close toPhoebe,taking very high-resolution photos of its surface and collecting data. On December 25, 2004, the Huygens probe separated from the Cassini probe before moving towards Titan's surface and landed on January 14, 2005. It landed on a dry surface, but it found that large bodies of liquid exist on the moon. The Cassini probe continued to collect data from Titan and a number of the icy moons. It found evidence that the moon Enceladus had water erupting from itsgeysers.[65]Cassini also proved, in July 2006, that Titan hadhydrocarbon lakes,located near its north pole. In March 2007, it discovered a large hydrocarbon lake the size of theCaspian Seanear its north pole.[66]

Cassini observedlightningoccurring in Saturn since early 2005. The power of the lightning was measured to be 1,000 times more powerful than lightning on Earth. Astronomers believe that the lightning observed in Saturn is the strongest ever seen.[67]

Notes[change|change source]

Related pages[change|change source]

References[change|change source]

  1. ↑Walter, Elizabeth (21 April 2003).Cambridge Advanced Learner's Dictionary(Second ed.). Cambridge University Press.ISBN978-0-521-53106-1.
  2. ↑"Saturnian".Oxford English Dictionary.Oxford University Press.2nd ed. 1989.
  3. ↑"Enabling Exploration with Small Radioisotope Power Systems"(PDF).NASA. September 2004. Archived fromthe original(PDF)on 22 December 2016.Retrieved26 January2016.
  4. ↑Müller; et al. (2010)."Azimuthal plasma flow in the Kronian magnetosphere".Journal of Geophysical Research.115(A8): A08203.Bibcode:2010JGRA..115.8203M.doi:10.1029/2009ja015122.
  5. ↑"Cronian".Oxford English Dictionary.Oxford University Press.2nd ed. 1989.
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  8. ↑Souami, D.; Souchay, J. (July 2012)."The solar system's invariable plane".Astronomy & Astrophysics.543:11.Bibcode:2012A&A...543A.133S.doi:10.1051/0004-6361/201219011.A133.
  9. ↑"HORIZONS Web-Interface".ssd.jpl.nasa.gov.
  10. ↑10.010.110.210.3Williams, David R. (23 December 2016)."Saturn Fact Sheet".NASA. Archived fromthe originalon 17 July 2017.Retrieved12 October2017.
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  12. ↑"NASA: Solar System Exploration: Planets: Saturn: Facts & Figures".Solarsystem.nasa.gov. 22 March 2011. Archived fromthe originalon 2 September 2011.Retrieved8 August2011.
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  51. ↑Rincon, Paul (July 1, 2005)."Saturn rings have own atmosphere".BBC News.London:BBC.RetrievedJune 19,2011.
  52. ↑Johnson, R.E. (2006)."The Enceladus and OH Tori at Saturn".SAO/NASA ADS Astronomy Abstract Service.644(2): L137–L139.Bibcode:2006ApJ...644L.137J.doi:10.1086/505750.S2CID37698445.RetrievedJune 19,2011.
  53. ↑53.053.1Malik, Tariq (2005-09-15)."Cassini Probe spies spokes in Saturn's rings".space.RetrievedApril 26,2011.
  54. ↑"Cassini exposes puzzles about ingredients in Saturn's rings".Cassini: unlocking Saturn's secrets.National Aeronautics and Space Administration. 2009-06-02. Archived fromthe originalon 2010-12-24.RetrievedMay 24,2011.
  55. ↑"Spoke's reappear on Saturn's rings".Astronomy Picture Of The Day.National Aeronautics and Space Administration. 2009-06-02.RetrievedApril 26,2011.
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  58. ↑Stott, Carole; Robert Dinwiddle, David Hughes and Giles Sparrow (2010).Space.DK Books. p. 161.ISBN978-0-7566-6738-2.RetrievedJune 20,2011.
  59. ↑McKay, Chris (2005-10-27)."Titan: a moon with atmosphere".Astrobiology Magazine.RetrievedJune 20,2011.
  60. ↑Zubrin, Robert (1999).Entering space: creating a spacefaring civilization.Section: Titan: Tarcher/Putnam. pp.163–166.ISBN978-1-58542-036-0.
  61. ↑61.061.1"Huygens".Solar System exploration.National Aeronautics and Space Administration. 2011. Archived fromthe originalon August 8, 2011.RetrievedApril 22,2011.
  62. ↑62.062.1Lloyd, James (2011-04-21)."Footprint detected from one of Saturn's moons".cosmosmagazine.Archived fromthe originalon July 4, 2011.RetrievedApril 21,2011.
  63. ↑"Aurora from Saturn moon 'circuit'".BBC News.BBC. 2011-04-21.RetrievedJuly 6,2011.
  64. ↑"The Pioneer 10 & 11 Spacecraft".Ames Research Center, NASA. October 8, 2005. Archived fromthe originalon January 30, 2006.RetrievedSeptember 13,2020.Mission Descriptions. Retrieved July 5, 2007.
  65. ↑"Radical! Liquid water on Enceladus".Science News.National Aeronautics and Space Administration. 2006-03-09. Archived fromthe originalon 2011-06-23.RetrievedJune 20,2011.
  66. ↑Rincon, Paul (March 14, 2007)."Probe reveals seas on Saturn moon".BBC News.London: BBC.RetrievedJune 20,2011.
  67. ↑"Astronomers find giant lightning storm at Saturn".sciencedaily.2006-02-15.RetrievedJune 20,2011.
  68. ↑Shirley, James H.; Fairbridge, Rhodes W. (1997).Encyclopedia of Planetary Sciences.New York: Springer. p. 62.ISBN978-0-412-06951-2.

Notes

  1. ↑1.01.11.21.31.41.51.61.7Refers to the level of 1 bar atmospheric pressure
  2. ↑Based on the volume within the level of 1 bar atmospheric pressure

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