|Aphelion||1,514.50 million km (10.1238 AU)|
|Perihelion||1,352.55 million km (9.0412 AU)|
|1,433.53 million km (9.5826 AU)|
Average orbital speed
|9.68 km/s (6.01 mi/s)|
|Known satellites||62 with formal designations; innumerable additional moonlets.|
|58,232 km (36,184 mi)[a]|
|0.687 g/cm3 (0.0248 lb/cu in)[b] (less than water)|
|0.210 I/MR2 estimate|
|35.5 km/s (22.1 mi/s)[a]|
Sidereal rotation period
|10h 33m 38s Template:+- |
Equatorial rotation velocity
|9.87 km/s (6.13 mi/s; 35,500 km/h)[a]|
|26.73° (to orbit)|
North pole right ascension
|40.589°; 2h 42m 21s|
North pole declination
|−0.55 to +1.17|
|14.5″ to 20.1″ (excludes rings)|
|59.5 km (37.0 mi)|
|Composition by volume||by volume:
Saturn is the sixth planet from the Sun in the Solar System. It is the second largest planet in the Solar System, after Jupiter. Saturn is one of the four gas giant planets, along with Jupiter, Uranus, and Neptune.
Inside Saturn is probably a core of iron, nickel, silicon and oxygen compounds, surrounded by a deep layer of metallic hydrogen, then a layer of liquid hydrogen and liquid helium and finally, an outer gaseous layer.
Saturn has 67 known moons orbiting the planet. 38 are officially named and 29 are waiting to be named. The largest moon is Titan, which is larger in volume than the planet Mercury. Titan is the second-largest moon in the Solar System. The largest moon is Jupiter's moon, Ganymede. There is also a very large system of rings around Saturn. These rings are made of ice with smaller amounts of rocks and dust. Some people believe that the rings were caused from a moon impact or other event. Saturn is about 1,433,000,000 km (869,000,000 mi) on average from the Sun. Saturn takes 29.6 Earth years to revolve around the Sun.
Physical features[change | change source]
Saturn is an oblate spheroid, meaning that it is flattened at the poles, and it swells out around its equator. The planet's equatorial diameter is 120,536 km (74,898 mi), while its polar diameter (the distance from the north pole to the south pole) is 108,728 km (67,560 mi); a 9% difference. Saturn has a flattened shape due to its very fast rotation, once every 10.8 hours.
Saturn is the only planet in the Solar System that is less dense than water. Even though the planet's core is very dense, it has a gaseous atmosphere, so the average specific density of the planet is 0.69 g/cm3. This means if Saturn could be placed in a large pool of water, it would float.
Atmosphere[change | change source]
Saturn's clouds show a banded pattern, like the cloud bands seen on Jupiter. Saturn's clouds are much fainter and the bands are wider at the equator. Saturn's lowest cloud layer is made up of water ice, and is about 10 km (6 mi) thick. The temperature here is quite low, at 250 K (-10°F, -23°C). However scientists do not agree about this. The layer above, about 77 km (48 mi) thick, is made up of ammonium hydrosulfide ice, and above that is a layer of ammonia ice clouds 80 km (50 mi) thick. The highest layer is made up of hydrogen and helium gases, which extends between 200 km (124 mi) and 270 km (168 mi) above the water cloud tops. Auroras are also known to form in Saturn in the mesosphere. The temperature at Saturn's cloud tops is extremely low, at 98 K (-283 °F, -175 °C). The temperatures in the inner layers are much higher than the outside layers because of the heat produced by Saturn's interior. Saturn's winds are some of the fastest in the Solar System, reaching 1,800 km/h (1,118 mph), ten times faster than winds on Earth.
Storms and spots[change | change source]
Saturn's atmosphere is also known to form oval shaped clouds, similar to the clearer spots seen in Jupiter. These oval spots are cyclonic storms, the same as cyclones seen on Earth. In 1990, the Hubble Space Telescope found a very large white cloud near Saturn's equator. Storms like the one in 1990 were known as Great White Spots. These unique storms only exist for a short time and only happen about every 30 Earth years, at the time of the summer solstice in the Northern Hemisphere. Great White Spots were also found in 1876, 1903, 1933, and 1960. If this cycle continues, another storm will form in about 2020.
The Voyager 1 spacecraft found a hexagonal cloud pattern near Saturn's north pole at about 78°N. The Cassini−Huygens probe later confirmed it in 2006. Unlike the north pole, the south pole does not show any hexagonal cloud feature. The probe also discovered a hurricane-like storm locked to the south pole that clearly showed an eyewall. Until this discovery, eyewalls had only been seen on Earth.
Interior[change | change source]
Saturn's interior is similar to Jupiter's interior. It has a small rocky core about the size of the Earth at its center. It is very hot; its temperature reaches 15,000 K (26,540 °F (14,727 °C)). Saturn is so hot that it gives out more heat energy into space than it receives from the Sun. 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. The core is heavy, with about 9 to 22 times more mass than the Earth's core.
Magnetic field[change | change source]
Saturn has a natural magnetic field that is weaker than Jupiter's. Like the Earth's, Saturn's field is a magnetic dipole. Saturn's field is unique in that it is perfectly symmetrical, unlike any other known planet. This means the field is exactly in line with the planet's axis. Saturn generates radio waves, but they are too weak to be detected from Earth. The moon Titan orbits in the outer part of Saturn's magnetic field and gives out plasma to the field from the ionised particles in Titan's atmosphere.
Rotation and orbit[change | change source]
Saturn's average distance from the Sun is over 1,400,000,000 km (869,000,000 mi), about nine times the distance from the Earth to the Sun. It takes 10,759 days, or about 29.8 years, for Saturn to orbit around the Sun. This is known as Saturn's orbital period.
Voyager 1 measured Saturn'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 interior. This is known as its rotational period.
Cassini measured the rotation of Saturn as being 10 hours 45 minutes 45 seconds ± 36 seconds. That is about six minutes, or one percent, longer than the radio rotational period measured by the Voyager 1 and Voyager 2 spacecraft, which flew by Saturn in 1980 and 1981.
Saturn's rotational period is calculated by the rotation speed of radio waves released by the planet. The Cassini−Huygens spacecraft discovered that the radio waves slowed down, suggesting that the rotational period increased. Since the scientists do not think Saturn's rotation is actually slowing down, the explanation may lie in the magnetic field that causes the radio waves.
Planetary rings[change | change source]
Saturn is best known for its planetary rings which are easy to see with a telescope. There are seven named rings; A, B, C, D, E, F, and G rings. They were named in the order they were discovered, which is different to their order from the planet. From the planet the rings are: D, C, B, A, F, G and E.:57
Scientists believe that the rings are material left after a moon broke apart.: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 also some of the moons, like Enceladus, which are thought to be made of ice.:61
History[change | change source]
The rings were first discovered by Galileo Galilei in 1610, using his telescope. They did not look like rings to Galileo, so he called them "handles". He thought that Saturn was three separate planets that almost touched one another. In 1612, when the rings were facing edge on with the Earth, the rings disappeared, then reappeared again in 1613, further confusing Galileo. In 1655, Christiaan Huygens was the first person to recognise Saturn was surrounded by rings. Using a much more powerful telescope than Galilei's, he noted Saturn "is surrounded by a thin, flat, ring, nowhere touching...". In 1675, Giovanni Domenico Cassini discovered that the planet's rings were in fact made of smaller ringlets with gaps. The largest ring gap was later named the Cassini Division. In 1859, James Clerk Maxwell showed 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. James Keeler studied the rings using a spectroscope in 1895 which proved Maxwell's theory.
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. 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 of silica rock, iron oxide and ice particles.: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.:58 These large waves are 500 m (1,640 ft) high, but only moving slowly at about 250 m (820 ft) each day.:58 Some scientists believe that the wave is caused by Saturn's moons. Another idea is the waves were made by a comet hitting Saturn in 1983 or 1984.:60
The largest gaps in the rings are the Cassini Division and the Encke Division, both visible from the Earth. The Cassini Division is the largest, measuring 4,800 km (2,983 mi) wide. 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 the gravitational force of some of Saturn's moons. The tiny moon Pan orbits inside Saturn's rings, creating a gap within the rings. Other ringlets keep their structure due to the gravitational force of shepherd satellites, such as Prometheus and Pandora. Other gaps form due to the gravitational force of a large moon farther away. The moon Mimas is responsible for clearing away the Cassini gap.
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's ultraviolet light breaks up the water ice in the rings. Chemical reaction also occurs between the ultraviolet light and the water molecules, creating hydrogen gas. The oxygen and hydrogen atmospheres around the rings are very widely spaced. As well as oxygen and hydrogen gas, the rings have a thin atmosphere made of hydroxide. This anion was discovered by the Hubble Space Telescope.
Spokes[change | change source]
The Voyager space probe discovered features shaped like rays, called spokes. These were also seen later by the Hubble telescope. The Cassini probe photographed the spokes in 2005. They are seen as dark when under sunlight, and appear light when against the unlit side. At first it was thought the spokes were made of microscopic dust particles but new evidence shows that they are made of ice. They rotate at the same time with the planet's magnetosphere, therefore, it is believed that they have a connection with electromagnetism. However, what causes the spokes to form is still unknown. They appear to be seasonal, disappearing during solstice and appearing again during equinox.
Moons[change | change source]
Saturn has 53 named moons, and another nine which are still being studied. 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). Seven moons are large enough to be a near perfect sphere caused by their own gravitation. These moons are Titan, Rhea, Iapetus, Dione, Tethys, Enceladus and Mimas. 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. Hyperion and Phoebe are the next largest moons, larger than 200 km (124 mi) in diameter.
In 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, then landed on Titan. Named after the Dutch astronomer Christiaan Huygens, it was the first spacecraft to land in the outer Solar System. The probe was designed to float in case it landed in liquid. Enceladus, the sixth largest moon, is about 500 km (311 mi) in diameter. It is one of the few outer solar system objects that shows volcanic activity. In 2011, scientists discovered an electric link between Saturn and Enceladus. This is caused by ionised particles from volcanos on the small moon interacting with Saturn's magnetic fields. Similar interactions cause the northern lights on Earth.
Exploration[change | change source]
Saturn was first explored by the Pioneer 11 spacecraft 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 in resolution. It discovered a new, thin ring called the F ring. It also discovered that the dark ring gaps appear bright when viewed towards the Sun, which shows the gaps are not empty of material. The spacecraft measured the temperature of the moon Titan.
In November 1980, Voyager 1 visited Saturn, and took higher resolution photographs of the planet, rings and moons. These photos were able to show the surface features of the moons. Voyager 1 went close to Titan, and gained much information about its atmosphere. In August, 1981, Voyager 2 continued to study the planet. Photos taken by the space probe showed that changes were happening to the rings and atmosphere. The Voyager spacecrafts discovered a number of moons orbiting close to Saturn's rings, as well as discovering new ring gaps.
On July 1, 2004, the Cassini−Huygens probe entered into orbit around Saturn. Before then, it flew close to Phoebe, 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 down towards Titan's surface and landed there 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 its geysers. Cassini also proved, in July 2006, that Titan had hydrocarbon lakes, located near its north pole. In March 2007, it discovered a large hydrocarbon lake the size of the Caspian Sea near its north pole.
Cassini observed lightning occurring 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.
Notes[change | change source]
- a Refers to the level of one bar atmospheric pressure
- b Orbital information is based on the barycentre of the Saturn system, the centre of mass, not the geometric centre. Barycentre measurements are used because they are not changed by the daily movement of the moons.
Related pages[change | change source]
References[change | change source]
- McCartney, Gretchen; Wendel, JoAnna (18 January 2019). "Scientists Finally Know What Time It Is on Saturn". NASA. Retrieved 18 January 2019.
- Mankovich, Christopher; et al. (17 January 2019). "Cassini Ring Seismology as a Probe of Saturn's Interior. I. Rigid Rotation". The Astrophysical Journal. 871 (1): 1. doi:10.3847/1538-4357/aaf798.
- Knecht, Robin (24 October 2005). "On The Atmospheres Of Different Planets" (PDF). Archived from the original (PDF) on 14 October 2017. Retrieved 14 October 2017.
- Brainerd, Jerome James 2004. "Giant gaseous planets". The Astrophysics Spectator. Retrieved 2010-07-05.
- "Planetary Satellite Discovery Circumstances". NASA. Retrieved 2019-12-28.
- "Cronia (Kronia)". Holidays, Festivals, and Celebrations of the World Dictionary. 2010. Retrieved 2011-07-11.
- Crystal, Ellie. "Saturn Mythology". Crystalinks.com. Retrieved 2007-02-28.
- "Saturn". Information Leaflet No. 42. Royal Greenwich Observatory. 2009. Retrieved 2011-04-26.
- "Cassini–Huygens Saturn arrival" (PDF). Press kit June 2004. National Aeronautics and Space Administration. p. 9. Retrieved 2011-06-25.
- Verba, Joan Marie (1991). Voyager: Exploring the outer planets. FTL Publications. p. 20. ISBN 0-9825232-0-3.
- "Saturn". MIRA: field trips to the stars: the Solar System. Monterey Institute of Research in Astronomy. 2006. Retrieved 2011-06-19. External link in
- "A gas giant with super-fast winds". Cassini: unlocking Saturn's secrets. National Aeronautics and Space Administration. 2007. Retrieved 2011-06-19.
- Wilkinson, John (2009). Probing the new solar system. CSIRO Publishing. p. 208. ISBN 978-0-643-09575-5. Retrieved 2011-05-23.
- Sullivant, Rosemary. "Saturn's storms run rings around Earth's". Cassini: unlocking Saturn's secrets. National Aeronautics and Space Administration. Retrieved 2011-05-24.
- S. Pérez-Hoyos, A. Sánchez-Lavega, R.G. French, J.F. Rojas. (2005). "Saturn's cloud structure and temporal evolution from ten years of Hubble Space Telescope images (1994–2003)". Science Direct. Retrieved 2011-06-19.CS1 maint: multiple names: authors list (link)
- "The 1990 Great White Spot of Saturn". 1993 Yearbook of Astronomy. W.W. Norton & Company, London. 1992. pp. 176–215.
- McKee, Maggie (2006-11-06). "Spectacular storm rages on Saturn's south pole". New Scientist Magazine. Retrieved 2011-04-21.
- "Saturn". Solar System. National Maritime Museum. 2005-10-04. Archived from the original on 2011-06-13. Retrieved 2011-06-19.
- Fortney, Jonathon J. (2004). "Looking into the giant planets". Science 305 (5689): 1414–1415. Retrieved 2007-04-30.
- Sutton, Christine (1981-08-27). "Saturn yields to Voyager's brief caress". New Scientist Magazine. Retrieved 2011-06-19.
- Smith, A. G.; Carr, T. D. (1959). "Radio-Frequency Observations of the Planets in 1957–1958". The Astrophysical Journal. 130: 641–647. doi:10.1086/146753.
- Russell C.T.; Luhmann J.G. (1997). "Saturn: magnetic field and magnetosphere". Encyclopedia of Planetary Sciences. New York: Chapman and Hall. pp. 718–719. Retrieved 2011-06-20.CS1 maint: multiple names: authors list (link)
- "NASA image of Saturn featured in Time Magazine's 'Year in Pictures'". NASA in your life. National Aeronautics and Space Administration. 2009-12-30. Retrieved 2011-06-24.
- "Saturn: orbital and rotational information". MIRA: field trips to the stars: the Solar System. Monterey Institute for Research in Astronomy. 2006. Retrieved 2011-07-06.
- Martinez, Carolina (2004-06-28). "Scientists find that Saturn's rotation period is a puzzle". Cassini: unlocking Saturn's secrets. National Aeronautics and Space Administration. Retrieved 2011-06-24.
- Lovett, Rick (June/July 2011). "Dance of the rings". Cosmos (39): 57. Retrieved 2011-06-21. Check date values in:
- Baalke, Ron (2005). "Historical background of Saturn's rings". www2.jpl.nasa.gov. National Aeronautics and Space Administration. Retrieved 2011-07-06.
- Maxwell, James Clerk (1859). "James Clerk Maxwell on the nature of Saturn's rings". www-history.mcs.st-andrews.ac.uk. Retrieved 2011-06-19.
- Brashear, Ronald (May 1999). "Christiaan Huygens and his Systema Saturnium". Smithsonian Institution Libraries. Retrieved 2011-04-19.
- "Saturn: Rings". Solar System exploration. National Aeronautics and Space Administration. 2011-03-22. Retrieved 2011-06-19.
- "StarChild: Saturn's Cassini Division". The Solar System. National Aeronautics and Space Administration. 2011. Retrieved 2011-06-19.
- Rincon, Paul (2005-07-01). "Saturn rings have own atmosphere". BBC News. London: British Broadcasting Corporation. Retrieved 2011-06-19.
- Johnson, R.E. (2006). "The Enceladus and OH Tori at Saturn". SAO/NASA ADS Astronomy Abstract Service. Retrieved 2011-06-19.
- Malik, Tariq (2005-09-15). "Cassini Probe spies spokes in Saturn's rings". space.com. Retrieved 2011-04-26.
- "Cassini exposes puzzles about ingredients in Saturn's rings". Cassini: unlocking Saturn's secrets. National Aeronautics and Space Administration. 2009-06-02. Retrieved 2011-05-24.
- "Spoke's reappear on Saturn's rings". Astronomy Picture Of The Day. National Aeronautics and Space Administration. 2009-06-02. Retrieved 2011-04-26.
- "Saturn: Moons". Solar System exploration: planets. National Aeronautics and Space Administration. 2011. Retrieved 2011-04-21.
- "About Saturn and its moons". Cassini Solstice Mission. National Aeronautics and Space Administration. 2011. Retrieved 2011-06-25.
- Stott, Carole; Robert Dinwiddle, David Hughes and Giles Sparrow (2010). Space. DK Books. p. 161. ISBN 978-0-7566-6738-2. Retrieved 2011-06-20.
- McKay, Chris (2005-10-27). "Titan: a moon with atmosphere". Astrobiology Magazine. Retrieved 2011-06-20.
- Zubrin, Robert (1999). Entering space: creating a spacefaring civilization. Section: Titan: Tarcher/Putnam. pp. 163–166. ISBN 978-1-58542-036-0.
- "Huygens". Solar System exploration. National Aeronautics and Space Administration. 2011. Archived from the original on 2011-08-08. Retrieved 2011-04-22.
- Lloyd, James (2011-04-21). "Footprint detected from one of Saturn's moons". cosmosmagazine.com. Archived from the original on 2011-07-04. Retrieved 2011-04-21.
- "Aurora from Saturn moon 'circuit'". BBC News. British Broadcasting Corporation. 2011-04-21. Retrieved 2011-07-06.
- "The Pioneer 10 & 11 Spacecraft". Ames Research Center, NASA. 2005-10-08. Archived from the original on 2006-01-30. Retrieved 2020-09-13. Mission Descriptions. Retrieved on 2007-07-05.
- "Radical! Liquid water on Enceladus". Science News. National Aeronautics and Space Administration. 2006-03-09. Retrieved 2011-06-20.
- Rincon, Paul (2007-03-14). "Probe reveals seas on Saturn moon". BBC News. London: British Broadcasting Corporation. Retrieved 2011-06-20.
- "Astronomers find giant lightning storm at Saturn". sciencedaily.com. 2006-02-15. Retrieved 2011-06-20.
- Shirley, James H.; Fairbridge, Rhodes W. (1997). Encyclopedia of Planetary Sciences. New York: Springer. p. 62. ISBN 978-0-412-06951-2.
- Refers to the level of 1 bar atmospheric pressure
- Based on the volume within the level of 1 bar atmospheric pressure
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- "Images of Saturn". spacetelescope.org. 2011. Retrieved 2011-06-19.
- "Saturn Earth comparison". Saturn fact Sheet. NASA. 2011. Retrieved 2011-06-19.
- Vladimir V. Tchernyi, Andrew Ju. Pospelov, Serge V. Girich (2009). "Studies on the Rings of Saturn". The Academy for Future Science. Retrieved 2011-06-19.CS1 maint: multiple names: authors list (link) Theoretical description of the rings of Saturn.
- "Eerie sounds of Saturn's radio emissions". Cassini: unlocking Saturn's secrets. NASA. 2008. Retrieved 2011-06-19. A WAV file of radio emissions from Saturn.
- "Bizarre hexagon on Saturn". News and Features. NASA. 2011. Retrieved 2011-06-19.