500 Words Essay On Saturn

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

How to say it/ˈsætərn/ ( listen)[1]
Orbit [4][b]
Reference dateJ2000
Longest distance from the Sun1,513,325,783 km
10.115 958 04 AU
Shortest distance from the Sun1,353,572,956 km
9.048 076 35 AU
Longest distance from the center of its orbital path
("semi-major axis")
1,433,449,370 km
9.582 017 20 AU
How long it takes to complete an orbit10,832.327 days
29.657 296 yr
How long an orbit seems to take
(from the central body)
378.09 days [2]
Average speed9.69 km/s [2]
Mean anomaly320.346 750°
Angle above the reference plane
2.485 240° to Ecliptic
5.51° to Sun’s equator
0.93° to Invariable plane[3]
Natural things which orbit itaround 200 observed (61 with secure orbits)
Size and other qualities
Average radius7007582320000000000♠58,232±6 km[5]
Surface area4.27×1010 km2[6][a]
83.703 Earths
Volume8.2713×1014 km3[2][a]
763.59 Earths
Mass5.6846×1026 kg [2]
95.152 Earths
Average density0.687 g/cm3[2][a]
(less than water)
Surface gravity10,44 m/s2[2][a]
0.914 g
Escape velocity35.5 km/s [2][a]
Turning speed9.87 km/s [a]
35 500 km/h
Angle at which it turns
(in relation to its orbit)
26.73° [2]
Angle above the celestial equator
83.537° [7]
How much light it reflects

0.342 bond

0.47 geom[2]
Seeming brightness
("apparent magnitude")
+1.2 to -0.24 [8]
Atmosphere [2]
Scale height59.5 km

~96% hydrogen (H2)
~3% helium
~0.4% methane
> 0.01% other

ammonium hydrosulfide (NH4SH)

Saturn is the sixth planet from the Sun in the Solar System. It is the second largest planet in the Solar System, after Jupiter. Like Jupiter, Uranus, and Neptune, Saturn is a "gas giant".

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 liquidhydrogen and liquid helium and finally, an outer gaseous layer.[9]

Saturn has 62 known moonsorbiting the planet; 53 are officially named.[10] 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. Saturn is about 1,400,000,000 km (869,000,000 mi) from the Sun. Saturn takes 29.6 Earth years to revolve around the Sun.[2]

Saturn was named after the Roman godSaturnus (called Kronos in Greek mythology).[11] Saturn's symbol is ♄ which is the symbol of Saturnus' sickle.[12]

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.[13] 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.[14] Saturn has a flattened shape; it is due to its very fast rotation, rotating once every 10.8 hours.[2]

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 (less than the density of water). This means if Saturn could be placed in a large pool of water, it would float.[15]

Atmosphere[change | change source]

The outer part of Saturn's atmosphere is made up of about 96% hydrogen, 3% helium, 0.4% methane and 0.01% ammonia.[2] There are also very small amounts of acetylene, ethane and phosphine.[16]

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.[16] 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.[16] 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.[16] 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.[17] Saturn's winds are some of the fastest in the Solar System, reaching 1,800 km/h (1,118 mph),[18] ten times faster than winds on Earth.[19]

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.[20] Great White Spots were also found in 1876, 1903, 1933, and 1960. If this cycle continues, another storm will form in about 2020.[21]

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.[22]

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 centre.[13] 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.[17] 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.[23] The core is heavy, with about 9 to 22 times more mass than the Earth's core.[24]

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.[25] This means the field is exactly in line with the planet's axis.[25] Saturn generates radio waves, but they are too weak to be detected from Earth.[26] 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.[27]

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 29.7 years, for Saturn to orbit around the Sun.[28] 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.[29] This is known as its rotational period.

Cassini measured the rotation of Saturn as being 10 hours 45 minutes 45 seconds ± 36 seconds.[30] 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.[30] 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.[30]

Planetary rings[change | change source]

Main article: Rings of Saturn

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.[31] 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.[31]:57

Scientists believe that the rings are material left after a moon broke apart.[31]: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.[31]: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.[32] 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...".[32] 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.[33]James Keeler studied the rings using a spectroscope in 1895 which proved Maxwell's theory.[34]

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.[31]: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.[31]:58 These large waves are 500 m (1,640 ft) high, but only moving slowly at about 250 m (820 ft) each day.[31]:58 Some scientists believe that the wave is caused by Saturn's moons.[35] Another idea is the waves were made by a comet hitting Saturn in 1983 or 1984.[31]: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.[36] 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.[36]

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.[37] 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.[38]

Spokes[change | change source]

The Voyager space probe discovered features shaped like rays, called spokes.[39] These were also seen later by the Hubble telescope. The Cassini probe photographed the spokes in 2005.[39] 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.[40] 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.[41]

Moons[change | change source]

Saturn has 53 named moons, and another nine which are still being studied.[42] 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).[43] 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.[44] 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.[45][46]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.[47] The probe was designed to float in case it landed in liquid.[47] 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.[48] 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.[48] Similar interactions cause the northern lights on Earth.[49]

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.[50]

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.[51] 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.[52]

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.[53]

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.[54]

Related pages[change | change source]

References[change | change source]

  1. Walter, Elizabeth 2003. Cambridge advanced learner's dictionary (2nd ed.). Cambridge University Press. ISBN 0521531063. 
  2., David R. 2006. "Saturn Earth comparison". Saturn fact sheet. National Aeronautics and Space Administration. Retrieved 2007-07-31. 
  3. Burša, Milan; Pĕc̆, Karel (1993). Gravity field and dynamics of the Earth. Springer. p. 301. ISBN 9783540568179. 
  4. Yeomans, Donald K. 2006. "HORIZONS System". Solar System dynamics. National Aeronautics and Space Administration. Retrieved 2007-08-08.  At the site, go to the "web interface" then select "Ephemeris Type", "Target Body: Saturn Barycenter" and "Center: Sun".
  5. ↑Seidelmann, P. Kenneth 2007. "Report of the IAU/IAG Working Group on cartographic coordinates and rotational elements: 2006". Celestial Mechanics and Dynamical Astronomy98 (3): 155–180. doi:10.1007/s10569-007-9072-y. 
  6. "Saturn". Solar System exploration: planets. National Aeronautics and Space Administration. 2011-03-22. Retrieved 2011-06-19. 
  7. ↑Seidelmann, P. Kenneth; Archinal, B. A.; A’hearn, M. F.; et al. (2007). "Report of the IAU/IAGWorking Group on cartographic coordinates and rotational elements: 2006". Celestial Mech. Dyn. Astr.90: 155–180. doi:10.1007/s10569-007-9072-y. http://adsabs.harvard.edu/doi/10.1007/s10569-007-9072-y. 
  8. Schmude, Richard W Junior (2001). "Wideband photoelectric magnitude measurements of Saturn in 2000". Georgia Journal of Science. Retrieved 2007-10-14. 
  9. Brainerd, Jerome James 2004. "Giant gaseous planets". The Astrophysics Spectator. Retrieved 2010-07-05. 
  10. Piazza, Enrico. Kirk Munsell, ed. "Saturn's moons". Cassini, Equinox Mission. JPL NASA. Retrieved 2010-06-22. 
  11. "Cronia (Kronia)". Holidays, Festivals, and Celebrations of the World Dictionary. 2010. Retrieved 2011-07-11. 
  12. Crystal, Ellie. "Saturn Mythology". Crystalinks.com. Retrieved 2007-02-28. 
  13. 13.013.1"Saturn". Information Leaflet No. 42. Royal Greenwich Observatory. 2009. Retrieved 2011-04-26. 
  14. "Cassini–Huygens Saturn arrival"(PDF). Press kit June 2004. National Aeronautics and Space Administration. p. 9. Retrieved 2011-06-25. 
  15. Verba, Joan Marie (1991). Voyager: Exploring the outer planets. FTL Publications. p. 20. ISBN 0982523203. 
  16."Saturn". MIRA: field trips to the stars: the Solar System. Monterey Institute of Research in Astronomy. 2006. Retrieved 2011-06-19. 
  17. 17.017.1"A gas giant with super-fast winds". Cassini: unlocking Saturn's secrets. National Aeronautics and Space Administration. 2007. Retrieved 2011-06-19. 
  18. Wilkinson, John (2009). Probing the new solar system. CSIRO Publishing. p. 208. ISBN 9780643095755. Retrieved 2011-05-23. 
  19. Sullivant, Rosemary. "Saturn's storms run rings around Earth's". Cassini: unlocking Saturn's secrets. National Aeronautics and Space Administration. Retrieved 2011-05-24. 
  20. 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. 
  21. "The 1990 Great White Spot of Saturn". 1993 Yearbook of Astronomy. W.W. Norton & Company, London. 1992. pp. 176–215. 
  22. McKee, Maggie (2006-11-06). "Spectacular storm rages on Saturn's south pole". New Scientist Magazine. Retrieved 2011-04-21. 
  23. "Saturn". Solar System. National Maritime Museum. 2005-10-04. Retrieved 2011-06-19. 
  24. Fortney, Jonathon J. (2004). "Looking into the giant planets". Science 305 (5689): 1414–1415. Retrieved 2007-04-30. 
  25. 25.025.1Sutton, Christine (1981-08-27). "Saturn yields to Voyager's brief caress". New Scientist Magazine. Retrieved 2011-06-19. 
  26. ↑Smith, A. G.; Carr, T. D. (1959). "Radio-Frequency Observations of the Planets in 1957–1958". The Astrophysical Journal130: 641–647. doi:10.1086/146753. 
  27. 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. 
  28. "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. 
  29. "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. 
  30., 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. 
  31., Rick (June/July 2011). "Dance of the rings". Cosmos (39): 57. http://www.cosmosmagazine.com/. Retrieved 2011-06-21. 
  32. 32.032.1Baalke, Ron (2005). "Historical background of Saturn's rings". www2.jpl.nasa.gov. National Aeronautics and Space Administration. Retrieved 2011-07-06. 
  33. 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. 
  34. Brashear, Ronald (May 1999). "Christiaan Huygens and his Systema Saturnium". Smithsonian Institution Libraries. Retrieved 2011-04-19. 
  35. "Saturn: Rings". Solar System exploration. National Aeronautics and Space Administration. 2011-03-22. Retrieved 2011-06-19. 
  36. 36.036.1"StarChild: Saturn's Cassini Division". The Solar System. National Aeronautics and Space Administration. 2011. Retrieved 2011-06-19. 
  37. Rincon, Paul (2005-07-01). "Saturn rings have own atmosphere". BBC News. London: British Broadcasting Corporation. Retrieved 2011-06-19. 
  38. Johnson, R.E. (2006). "The Enceladus and OH Tori at Saturn". SAO/NASA ADS Astronomy Abstract Service. Retrieved 2011-06-19. 
  39. 39.039.1Malik, Tariq (2005-09-15). "Cassini Probe spies spokes in Saturn's rings". space.com. Retrieved 2011-04-26. 
  40. "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
Saturn compared with the size of the Earth
The spokes in Saturn's rings, photographed by Voyager 2
Saturn as seen from the Cassini spacecraft in 2007
Drawing of Cassini in orbit around Saturn

Students explore Saturn and its moons in the Cassini competition

12 May 2017

Since its arrival at Saturn in 2004, the international Cassini-Huygens mission has made numerous discoveries about the beautiful planet, its fascinating rings, and mysterious moons. The stunning images of the Saturnian system taken by the Cassini spacecraft provide the inspiration behind the ‘Cassini scientist for a day’ competition that is designed to give school students a taste of life as a space scientist. Over 1400 students from across Europe participated in the 2016–2017 competition and the winners have now been selected.

'Cassini scientist for a day' is an international competition, with students from all over the world taking part. NASA/JPL runs the contest in the United States, while ESA coordinates the competition in Europe, with a national organiser and a panel of judges in each country that competes.

To enter, students needed to first research three selected scientific targets imaged by the Cassini spacecraft over the past few years. Students then chose the one target that they thought was the most scientifically interesting and wrote a 500-word essay describing why.

For the 2016-2017 competition, students could choose between: ice plumes at the south pole of Enceladus, the lakes of Titan, and the hexagon at Saturn's north pole.

Target 1. Ice plumes at the south pole of Enceladus.
Credit: NASA/JPL/Space Science Institute.
Target 2. The lakes of Titan.
Credit: NASA/JPL/Space Science Institute.
Target 3. The hexagon at Saturn's north pole.
Credit: NASA/JPL/Space Science Institute.

A full list of European winners can be found here.

More than 1400 students entered the competition, some of them collaborating in teams of up to four people. Each participating country selected their national winners, all of whom will receive a selection of ESA gifts, as well as having their essays published on the ESA website. All participants will receive a certificate recognising their contribution to the competition.

The Cassini-Huygens mission

Artist's impression of Cassini at Saturn. Credit: NASA.

The Cassini–Huygens mission is a cooperative project of NASA, ESA and the Italian Space Agency (ASI). Launched in 1997, the Cassini-Huygens spacecraft arrived in the Saturn system in July 2004. On 25 December 2004, the Huygens probe was released from the orbiter and parachuted through the atmosphere to land on the surface of Saturn's largest moon, Titan, on 14 January 2005.

After more than a decade of ground-breaking discoveries, orbiting Saturn and providing scientists with an abundance of information about the giant planet and its moons, Cassini is approaching its end. Now in its final phase, the last orbits of Cassini will be spectacular. The spacecraft will orbit close to Saturn and its rings, before taking a final plunge into Saturn’s atmosphere on 15 September 2017. Over its 13-year mission, Cassini will have covered about half of Saturn’s orbit, in which the planet takes 29 years to circle the Sun.


Last Update: 15 August 2017


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