Download presentation on the topic Saturn. Presentation on the topic "Saturn"

Description of the presentation by individual slides:

1 slide

Slide description:

2 slide

Slide description:

Orbital characteristics Aphelion 1,513,325,783 km Perihelion 1,353,572,956 km Semi-major axis 1,433,449,370 km Orbital eccentricity 0.055 723,219 Sidereal period 10,832.327 days Synodic period 378.09 days Orbital speed 9.69 km/s (average) Inclination 2.485 240° 5.51° (relative to the solar equator) Longitude of the ascending node 113.642 811° Periapsis argument 336.013 862° Number of satellites 61

3 slide

Slide description:

Physical characteristics Compression 0.097 96 ± 0.000 18 Equatorial radius 60,268 ± 4 km Polar radius 54,364 ± 10 km Surface area 4.27 × 1010 km² Volume 8.2713 × 1014 km³ Weight 5.6846 × 1026 kg Average density 0.687 g /cm³ Acceleration of gravity at the equator 10 .44 m/s² Second escape velocity 35.5 km/s Rotation speed (at the equator) 9.87 km/s Rotation period 10 hours 34 minutes 13 seconds plus or minus 2 seconds Rotation axis inclination 26.73° North pole declination 83.537° Albedo 0.342 (Bond) 0.47 (geom.albedo)

4 slide

Slide description:

5 slide

Slide description:

Saturn is the sixth planet from the Sun and the second largest planet in the Solar System after Jupiter. Saturn, as well as Jupiter, Uranus and Neptune, are classified as gas giants. Saturn is named after the Roman god Saturn, the counterpart of the Greek Kronos (Titan, father of Zeus) and the Babylonian Ninurta. Saturn's symbol is a sickle (Unicode: ♄). Saturn is mostly hydrogen, with some helium and traces of water, methane, ammonia and “rocks.” The inner region is a small core of rock and ice, covered with a thin layer of metallic hydrogen and a gaseous outer layer. The planet's outer atmosphere appears calm and serene, although it occasionally exhibits some long-lasting features. The wind speed on Saturn can reach 1800 km/h in places, which is significantly higher than, for example, on Jupiter. Saturn has a planetary magnetic field that is intermediate in power between the Earth's magnetic field and the powerful field of Jupiter. Saturn's magnetic field extends 1 million km in the direction of the Sun. The shock wave was detected by Voyager 1 at a distance of 26.2 Saturn radii from the planet itself, the magnetopause is located at a distance of 22.9 radii.

6 slide

Slide description:

Saturn has a noticeable ring system consisting mainly of ice particles, smaller quantity rocks and dust. There are 61 currently known satellites orbiting the planet. Titan is the largest of them, as well as the second largest satellite in the Solar System (after the satellite of Jupiter, Ganymede), which is larger than the planet Mercury and has the only dense atmosphere among the many satellites of the Solar System.

7 slide

Slide description:

Saturn's upper atmosphere is composed of 93% hydrogen (by volume) and 7% helium (compared to 18% in Jupiter's atmosphere). There are impurities of methane, water vapor, ammonia and some other gases. Ammonia clouds in the upper part of the atmosphere are more powerful than Jovian clouds. According to Voyagers, strong winds blow on Saturn; the devices recorded air flow speeds of 500 m/s. Winds blow mainly in the eastern direction (in the direction of axial rotation). Their strength weakens with distance from the equator; As we move away from the equator, westerly atmospheric currents also appear. A number of data indicate that the winds are not limited to the cloud top layer, but must extend inward for at least 2 thousand km. In addition, Voyager 2 measurements showed that the winds in the southern and northern hemispheres are symmetrical relative to the equator. There is an assumption that the symmetrical flows are somehow connected under the layer of visible atmosphere. In the atmosphere of Saturn, stable formations sometimes appear that are super-powerful hurricanes. Similar objects are observed on other gas planets of the Solar System (Great Red Spot on Jupiter, Great Dark Spot on Neptune). A giant "Great White Oval" appears on Saturn about once every 30 years, last seen in 1990 (smaller hurricanes form more often). Today, such an atmospheric phenomenon of Saturn as the “Giant Hexagon” remains not fully understood. It is a stable formation in the form of a regular hexagon with a diameter of 25 thousand kilometers, which surrounds the north pole of Saturn. Powerful lightning discharges have been detected in the atmosphere, auroras, ultraviolet radiation hydrogen. In particular, on August 5, 2005, the Cassini spacecraft detected radio waves caused by lightning. Atmosphere

8 slide

Slide description:

Exploring Saturn Saturn is one of the five planets in the solar system that are easily visible to the naked eye from Earth. At maximum, Saturn's brilliance exceeds first magnitude. Observing Saturn for the first time through a telescope in 1609-1610, Galileo Galilei noticed that Saturn did not look like a single celestial body, but like three bodies almost touching each other, and suggested that they were two large satellites. Two years later, Galileo repeated the observations and, to his amazement, found no satellites. In 1659, Huygens, using a more powerful telescope, found that the “companions” are actually a thin flat ring encircling the planet and not touching it. Huygens also discovered Saturn's largest moon, Titan. Since 1675, Cassini has been studying the planet. He noticed that the ring consists of two rings, separated by a clearly visible gap - the Cassini gap, and discovered several more large satellites of Saturn.

Slide 9

Slide description:

In 1997, the Cassini-Huygens spacecraft was launched towards Saturn and, after seven years of flight, on July 1, 2004, it reached the Saturn system and entered orbit around the planet. The main objectives of this mission, designed for a minimum of 4 years, are to study the structure and dynamics of the rings and satellites, as well as to study the dynamics of the atmosphere and magnetosphere of Saturn. In addition, the special Huygens probe separated from the apparatus and parachuted down to the surface of Saturn's moon Titan. In 1979, the Pioneer 11 spacecraft made its first flyby of Saturn, followed by Voyager 1 and Voyager 2 in 1980 and 1981. These devices first discovered the magnetic field of Saturn and explored its magnetosphere, observed storms in the atmosphere of Saturn, obtained detailed images of the structure of the rings and determined their composition. In the 1990s, Saturn, its moons and rings were repeatedly studied by the Hubble Space Telescope. Long-term observations provided a lot of new information that was not available to Pioneer 11 and Voyagers during their one-time flyby of the planet.

10 slide

Slide description:

Saturn's moons The moons are named after the heroes of ancient myths about titans and giants. Almost all of these cosmic bodies are light. The largest satellites develop an internal rocky core. The name “ice” satellites most closely matches the satellites of Saturn. Some of them have an average density of 1.0 g/cm3, which is more consistent with water ice. The density of others is slightly higher, but also small (Titan is an exception). Until 1980, ten satellites of Saturn were known. Since then, several more have been opened. One part was discovered as a result of telescopic observations in 1980, when the ring system was visible edge-on (and thanks to this, observations were not interfered with by bright light), and the other was discovered during flybys of Voyager 1 and 2 in 1980 and 1981. After which the planet had 17 satellites.

11 slide

Slide description:

In 1990, the 18th satellite was discovered, and in 2000, 12 more small satellites were discovered, apparently captured by the planet of asteroids. At the end of 2004, Hawaiian astronomers discovered 12 more new satellites irregular shape with a diameter of 3 to 7 kilometers using the Cassini spacecraft. The capture version is confirmed by the fact that 11 of the 12 bodies orbit the planet in a direction different from that of the “main” satellites. This is also evidenced by the strong elongation and exceptionally large - about 20 million kilometers - diameter of the orbits. During 2006, a team of scientists led by David Jewitt from the University of Hawaii, working at the Japanese Subaru Telescope in Hawaii, announced the discovery of 9 moons of Saturn (In total, Jewitt's team has discovered 21 moons of Saturn since 2004). In the first half of 2007, 5 more satellites were added, bringing the total to 60. On August 15, 2008, a study of images taken by Cassini during a 600-day study of Saturn's G ring revealed the 61st satellite.

12 slide

Slide description:

The rings of Saturn are visible from Earth through a small telescope. They are made up of thousands and thousands of small solid particles of rock and ice that orbit the planet. There are 3 main rings, named A, B and C. They are visible without much trouble from Earth. There are also weaker rings - D, E, F. Upon closer examination, there are a great many rings. There are gaps between the rings where there are no particles. The one of the gaps that can be seen with an average telescope from Earth (between rings A and B) is called the Cassini gap. On clear nights, you can even see less visible cracks. The inner parts of the rings rotate faster than the outer ones.

Slide 13

Slide description:

The width of the rings is 400 thousand km, but their thickness is only a few tens of meters. Stars can be seen through the rings, although their light is noticeably weakened. All rings consist of individual pieces of ice different sizes: from dust particles to several meters in diameter. These particles move at almost identical speeds (about 10 km/s), sometimes colliding with each other. Under the influence of satellites, the ring bends slightly, ceasing to be flat: shadows from the Sun are visible. The plane of the rings is inclined to the orbital plane by 29°. Therefore, during the year we see them as wide as possible, after which their apparent width decreases, and, after about 15 years, they turn into a faintly distinguishable feature. The rings of Saturn have constantly excited the imagination of researchers with their unique shape. Kant was the first to predict the existence of the fine structure of Saturn's rings. During the 20th century, new data on planetary rings was gradually accumulated: estimates of the size and concentration of particles in the rings of Saturn were obtained, spectral analysis established that the rings are icy, and the mysterious phenomenon of azimuthal variability in the brightness of Saturn's rings was discovered.

Slide 14

Slide description:

Interesting Facts There is no solid surface on Saturn. The planet's average density is the lowest in the Solar System. The planet consists mainly of hydrogen and helium, the two lightest elements in space. The planet's density is only 0.69 that of water. This means that if there were an ocean of the appropriate size, Saturn would float on its surface. The robotic Cassini spacecraft, which is currently (October 2008) orbiting Saturn, has transmitted images of the planet's northern hemisphere. Since 2004, when Cassini flew up to it, noticeable changes have occurred, and it is now painted in unusual colors. The reasons for this are not yet clear. Although it is not yet known why Saturn's colors arose, it is believed that the recent change in colors is due to the changing seasons. The clouds on Saturn form a hexagon - a giant hexagon. First discovered during Voyager's flybys of Saturn in the 1980s, a similar phenomenon has never been observed anywhere else in the solar system. If Saturn's south pole with its spinning hurricane doesn't seem strange, then the north pole may be considered much more unusual. Strange cloud structure captured in infrared image spacecraft Cassini in October 2006. The images show that the hexagon remained stable in the 20 years following Voyager's mission. Movies showing Saturn's north pole show the clouds maintaining a hexagonal structure as they rotate. Individual clouds on Earth may have a hexagonal shape, but unlike them, the cloud system on Saturn has six well-defined sides of almost equal length. Four Earths can fit inside this hexagon. There is no complete explanation for this phenomenon yet.

15 slide

Slide description:

Literature: Wivipedia BEKiM Other Internet resources British astronomers have discovered a new type of aurora in the atmosphere of Saturn. On November 12, 2008, cameras on the Cassini spacecraft captured infrared images of Saturn's north pole. In these images, researchers discovered auroras that have never been observed before in the solar system. In the image, these unique auroras are colored blue, and the clouds below are colored red. The image shows a previously discovered hexagonal cloud directly below the auroras. The auroras on Saturn can cover the entire pole, while on Earth and Jupiter the aurora rings, being driven by the magnetic field, only surround the magnetic poles. The familiar ring auroras were also observed on Saturn. Recently captured unusual auroras over Saturn's north pole changed significantly within minutes. The changing nature of these auroras indicates that the variable flow of charged particles from the Sun is affected by some magnetic forces that were not previously suspected.

Municipal educational institution "Russian-Ustinskaya basic secondary school"

Completed:

4th grade student

Kiselev Serezha

Classroom teacher:

Kiseleva N.P.

Completed by an 11th grade student

Municipal educational institution "Pushninskaya Secondary School"

Konovalova M.

year 2014

Saturn- the sixth planet from the Sun and the second largest planet in the Solar System after Jupiter.

Saturn is named after the Roman god Saturn,

The symbol of Saturn is the sickle

Saturn exploration

Observing Saturn for the first time through a telescope in 1609-1610, Galileo Galilei noticed that Saturn appeared as three bodies almost touching each other, and suggested that these were two large “companions” (satellites) of Saturn.

Two years later, Galileo repeated the observations and, to his amazement, found no satellites.

There is no solid surface on Saturn.
The planet consists mainly of hydrogen and helium, the two lightest elements in space.
The clouds on Saturn form a hexagon.
British astronomers have discovered a new type of aurora in Saturn's atmosphere, which forms a ring around one of the planet's poles.

Completed by an 11th grade student

Municipal educational institution "Pushninskaya Secondary School"

Konovalova M.

Thank you for your attention

Completed by an 11th grade student

Municipal educational institution "Pushninskaya Secondary School"

Slide 1

Planets of the solar system
Saturn
Completed by: Stasyuk N. MBOU Kolybelskaya secondary school, grade 11, 2009

Slide 2

Orbital characteristics Orbital characteristics
Aphelion 1,513,325,783 km
Perihelion 1,353,572,956 km
Semi-major axis 1,433,449,370 km
Orbital eccentricity 0.055 723 219
Sidereal period 10,832.327 days
Synodic period 378.09 days
Orbital speed 9.69 km/s (average)
Inclination 2.485 240° 5.51° (relative to solar equator)
Longitude of the ascending node 113.642 811°
Periapsis argument 336.013 862°
Number of satellites 61

Slide 3

Physical characteristics Physical characteristics
Compression 0.097 96 ± 0.000 18
Equatorial radius 60,268 ± 4 km
Polar radius 54,364 ± 10 km
Surface area 4.27×1010 km²
Volume 8.2713×1014 km³
Weight 5.6846×1026 kg
Average density 0.687 g/cm³
Gravity acceleration at the equator 10.44 m/s²
Second escape velocity 35.5 km/s
Rotation speed (at the equator) 9.87 km/s
Rotation period 10 hours 34 minutes 13 seconds plus or minus 2 seconds
Rotation axis tilt 26.73°
Declination at the North Pole 83.537°
Albedo 0.342 (Bond) 0.47 (geom.albedo)

Slide 4

Slide 5

Slide 6

Saturn has a prominent ring system made up primarily of ice particles and smaller amounts of rock and dust. There are 61 currently known satellites orbiting the planet. Titan is the largest of them, as well as the second largest satellite in the Solar System (after the satellite of Jupiter, Ganymede), which is larger than the planet Mercury and has the only dense atmosphere among the many satellites of the Solar System.

Slide 7

In the atmosphere of Saturn, stable formations sometimes appear that are super-powerful hurricanes. Similar objects are observed on other gas planets of the Solar System (Great Red Spot on Jupiter, Great Dark Spot on Neptune). A giant "Great White Oval" appears on Saturn about once every 30 years, last seen in 1990 (smaller hurricanes form more often). Today, such an atmospheric phenomenon of Saturn as the “Giant Hexagon” remains not fully understood. It is a stable formation in the form of a regular hexagon with a diameter of 25 thousand kilometers, which surrounds the north pole of Saturn.

Powerful lightning discharges, auroras, and ultraviolet hydrogen radiation have been detected in the atmosphere. In particular, on August 5, 2005, the Cassini spacecraft detected radio waves caused by lightning.
Saturn is one of the five planets in the solar system that are easily visible to the naked eye from Earth. At maximum, Saturn's brilliance exceeds first magnitude.

Observing Saturn for the first time through a telescope in 1609-1610, Galileo Galilei noticed that Saturn did not look like a single celestial body, but like three bodies almost touching each other, and suggested that they were two large satellites. Two years later, Galileo repeated the observations and, to his amazement, found no satellites.

In 1659, Huygens, using a more powerful telescope, found that the “companions” are actually a thin flat ring encircling the planet and not touching it. Huygens also discovered Saturn's largest moon, Titan. Since 1675, Cassini has been studying the planet. He noticed that the ring consists of two rings, separated by a clearly visible gap - the Cassini gap, and discovered several more large satellites of Saturn.
Slide 9

In 1997, the Cassini-Huygens spacecraft was launched towards Saturn and, after seven years of flight, on July 1, 2004, it reached the Saturn system and entered orbit around the planet. The main objectives of this mission, designed for a minimum of 4 years, are to study the structure and dynamics of the rings and satellites, as well as to study the dynamics of the atmosphere and magnetosphere of Saturn. In addition, the special Huygens probe separated from the apparatus and parachuted down to the surface of Saturn's moon Titan.

Slide 11

In 1990, the 18th satellite was discovered, and in 2000, 12 more small satellites were discovered, apparently captured by the planet of asteroids. At the end of 2004, Hawaiian astronomers discovered 12 more new satellites of irregular shape with a diameter of 3 to 7 kilometers using the Cassini spacecraft. The capture version is confirmed by the fact that 11 of the 12 bodies orbit the planet in a direction different from that of the “main” satellites. This is also evidenced by the strong elongation and exceptionally large - about 20 million kilometers - diameter of the orbits. During 2006, a team of scientists led by David Jewitt from the University of Hawaii, working at the Japanese Subaru Telescope in Hawaii, announced the discovery of 9 moons of Saturn (In total, Jewitt's team has discovered 21 moons of Saturn since 2004). In the first half of 2007, 5 more satellites were added, bringing the total to 60. On August 15, 2008, a study of images taken by Cassini during a 600-day study of Saturn's G ring revealed the 61st satellite.

Slide 12

Slide 13

The width of the rings is 400 thousand km, but their thickness is only a few tens of meters. Stars can be seen through the rings, although their light is noticeably weakened. All rings consist of individual pieces of ice of different sizes: from specks of dust to several meters in diameter. These particles move at almost identical speeds (about 10 km/s), sometimes colliding with each other. Under the influence of satellites, the ring bends slightly, ceasing to be flat: shadows from the Sun are visible. The plane of the rings is inclined to the orbital plane by 29°. Therefore, during the year we see them as wide as possible, after which their apparent width decreases, and, after about 15 years, they turn into a faintly distinguishable feature. The rings of Saturn have constantly excited the imagination of researchers with their unique shape. Kant was the first to predict the existence of the fine structure of Saturn's rings. During the 20th century, new data on planetary rings was gradually accumulated: estimates of the size and concentration of particles in the rings of Saturn were obtained, spectral analysis established that the rings are icy, and the mysterious phenomenon of azimuthal variability in the brightness of Saturn's rings was discovered.

Slide 14

Interesting Facts
There is no solid surface on Saturn. The planet's average density is the lowest in the Solar System. The planet consists mainly of hydrogen and helium, the two lightest elements in space. The planet's density is only 0.69 that of water. This means that if there were an ocean of the appropriate size, Saturn would float on its surface.
The robotic Cassini spacecraft, which is currently (October 2008) orbiting Saturn, has transmitted images of the planet's northern hemisphere. Since 2004, when Cassini flew up to it, noticeable changes have occurred, and it is now painted in unusual colors. The reasons for this are not yet clear. Although it is not yet known why Saturn's colors arose, it is believed that the recent change in colors is due to the changing seasons.
The clouds on Saturn form a hexagon - a giant hexagon. First discovered during Voyager's flybys of Saturn in the 1980s, a similar phenomenon has never been observed anywhere else in the solar system. If Saturn's south pole with its spinning hurricane doesn't seem strange, then the north pole may be considered much more unusual. The strange cloud structure was captured in an infrared image by the Cassini spacecraft in October 2006. The images show that the hexagon remained stable in the 20 years following Voyager's mission. Movies showing Saturn's north pole show the clouds maintaining a hexagonal structure as they rotate. Individual clouds on Earth may have a hexagonal shape, but unlike them, the cloud system on Saturn has six well-defined sides of almost equal length. Four Earths can fit inside this hexagon. There is no complete explanation for this phenomenon yet.

Slide 15

Literature: Wivipedia BEKiM Other Internet resources
British astronomers have discovered a new type of aurora in Saturn's atmosphere. On November 12, 2008, cameras on the Cassini spacecraft captured infrared images of Saturn's north pole. In these images, researchers discovered auroras that have never been observed before in the solar system. In the image, these unique auroras are colored blue, and the clouds below are colored red. The image shows a previously discovered hexagonal cloud directly below the auroras. The auroras on Saturn can cover the entire pole, while on Earth and Jupiter the aurora rings, being driven by the magnetic field, only surround the magnetic poles. The familiar ring auroras were also observed on Saturn. Recently captured unusual auroras over Saturn's north pole changed significantly within minutes. The changing nature of these auroras indicates that the variable flow of charged particles from the Sun is affected by some magnetic forces that were not previously suspected.

The sixth planet from the Sun and the second largest planet in the Solar System after Jupiter.

PARAMETERS OF THE PLANET The time for a complete revolution of the planet around the Sun is 29.7 years. A day on Saturn is 10 hours and 15 minutes. Like all planets in the Solar System, its orbit is not a perfect circle, but has an elliptical trajectory. The average distance to the Sun is 1.43 billion km, or 9.58 AU+. The closest point in Saturn’s orbit is called perihelion and is located 9 astronomical units from the Sun.

The most distant point of the orbit is called aphelion and is located 10.1 astronomical units from the Sun.

Saturn is a type of gas planet: it consists mainly of gases and does not have a solid surface. The equatorial radius of the planet is 60,300 km, the polar radius is 54,400 km; Of all the planets in the solar system, Saturn has the greatest compression. The mass of the planet is 95.2 times higher, but the average density of Saturn is only 0.687 g/cm3, which makes it the only planet in the solar system whose average density is less than that of water. Therefore, although the masses of Jupiter and Saturn differ by more than 3 times, their equatorial diameter differs by only 19%. The density is much higher (1.27-1.64 g/cm3). The acceleration of gravity at the equator is 10.44 m/s², which is comparable to the values of Earth and Neptune, but much less than that of Jupiter. the rest of the Earth, the mass of gas giants

ATMOSPHERE Saturn's upper atmosphere consists of 96.3% hydrogen (by volume) and 3.25% helium (compared to 10% in Jupiter's atmosphere). There are impurities of methane, ammonia, phosphine, ethane and some other gases. Ammonia clouds in the upper part of the atmosphere are more powerful than Jovian clouds. Clouds in the lower atmosphere are composed of ammonium hydrosulfide (NH4SH) or water.

RINGS OF SATURN Saturn is one of the most mysterious planets for both professional astronomers and amateurs. Much of the interest in the planet comes from the distinctive rings around Saturn. Although they are not visible to the naked eye, the rings can be seen even with a weak telescope.

Made mostly of ice, Saturn's rings are held in orbit by the complex gravitational influences of the gas giant and its moons, some of which are actually rings. Although people have learned a lot about rings since they were first discovered 400 years ago, this knowledge is constantly being added to (for example, the most distant ring from the planet was discovered only ten years ago). are within

SATELLITES remain the main ones today. The largest satellites - Mimas, Enceladus, Tethys, Dione, Rhea, Titan and Iapetus - were discovered by 1789, but are still objects of research today. The diameters of these satellites vary from 397 (Mimas) to 5150 km (Titan), the semi-major axis of the orbit from 186 thousand km (Mimas) to 3561 thousand km (Iapetus). The mass distribution corresponds to the diameter distribution. Titan has the greatest orbital eccentricity, Dione and Tethys have the least. All satellites with known synchronous orbits, which leads to their gradual removal. parameters are above

TITAN and structure The largest of the satellites is Titan. It is also the second largest in the Solar System as a whole, after Jupiter's moon Ganymede. Titan is made up of about half water ice and half rock. This composition is similar to some of the other large satellites of the gas planets, but Titan is very different from them, being predominantly nitrogen in composition, there is also a small amount of methane and ethane that form clouds. Titan is also the only body in the Solar System, besides the Earth, for which the existence of liquid on the surface has been proven. The possibility of the emergence of simple organisms is not excluded by scientists. Titan's diameter is 50% larger than that of the Moon. It is also larger than the planet Mercury, although inferior to it in mass. atmosphere, its

1 slide

2 slide

Saturn Saturn is the sixth planet from the Sun and the second largest planet in the Solar System after Jupiter.

The average radius of Saturn is 9.1 times that of Earth. In the earth's sky, Saturn looks like a yellowish star. Even with the help of a non-professional telescope, you can easily see the distinct rings surrounding Saturn, one of the features of this planet. Saturn has 62 moons, some of which were discovered relatively recently. The largest of them are: Atlas (radius 20 km), Pandora (70 km); Prometheus (55 km), Epimetheus (70 km), Janus (110 km), Mimas (196 km), Enceladus (250 km), Tethys (530 km), Telesto (17 km), Calypso (17 km), Dione ( 560 km), 198 S6 (18 km), Rhea (754 km), Titan (2575 km), Hyperion (205 km), Iapetus (730 km), Phoebe (110 km). Almost all moons (except Titan) are composed primarily of ice and rock. The surface of Saturn's moons is covered with many craters - evidence of numerous collisions with asteroids.

4 slide

The main attraction of Saturn is its clearly visible ring system. From afar, the ring appears to be a single ring, but more powerful telescopes and research have made it possible to determine that there are actually several rings. To date, the presence of 7 rings has already been definitely established. Saturn's rings consist of a huge number of small rock and ice particles, the composition of which is not fully determined. There are several different versions about the origin of these rings. According to one of them, these are the remains of one of Saturn’s satellites, which was destroyed as a result of a collision with another cosmic body. Characteristics: Mass 5.7 1026 kg Diameter 120,536 km Density 0.69 g/cm3 Period of rotation around its axis 10 hours 23 minutes Orbital period 29.46 years Average distance from the Sun 1,426.98 million km average speed orbital movement 9.65 km/sec Gravity acceleration 11.3 m/s2 Direction of rotation direct Volume 0.305 1023 m3 Distance from Earth from 1,199 million to 1,653 million km