give information about saturn?

Answer 1

Saturn is an oblate spheroid, i.e. it is flattened at the poles and bulges at the equator; its equatorial and polar diameters vary by almost 10% (120,536 km vs. 108,728 km). This is the result of its rapid rotation and fluid state. The other gas planets are also oblate, but to a lesser degree. Saturn is the only planet of the Solar System that is less dense than water. Although Saturn's core is considerably more dense than water, the average specific density of the planet is 0.69 due to the gaseous atmosphere.

For the rest of the info refer

http://en.wikipedia.org/wiki/Saturn

Answer 2

Go to your library and check out last month's National Geographic (the one with Saturn on the cover). It has some of the most up to date info and some amazing photos. just read it last night and was fascinated.

Answer 3

SATURN IS THE SIXTH PLANET FROM THE SUN.IT IS A GAS GIANT,THE SECOND LARGEST PLANET IN THE SOLAR SYSTEM AFTER JUPITER.SATURN HAS A PROMINENT SYSTEM OF RINGS,CONSISTING MOSTLY OF ICE PARTICLES WITH A SMALLER AMOUNT OF ROCKY DEBRIS AND DUST.IT WAS NAMED AFTER THE ROMAN GOD SATURN(THE GREEK EQUIVALENT IS KRONOS,FATHER OF ZEUS)ITS SYMBOL IS A STYLIZED REPRESENTATION OF THE GOD'S SICKLE.

Answer 4

Saturn (IPA: /ˈsatən, -əː(r)n/) is the sixth planet from the Sun. It is a gas giant (also known as a Jovian planet, after the planet Jupiter), the second-largest planet in the solar system after Jupiter. Saturn has a prominent system of rings, consisting mostly of ice particles with a smaller amount of rocky debris and dust. It was named after the Roman god Saturn (the Greek equivalent is Kronos, father of Zeus). Its symbol is a stylized representation of the god's sickle
Saturn's interior is similar to Jupiter's, having a rocky core at the center, a liquid metallic hydrogen layer above that, and a molecular hydrogen layer above that. Traces of various ices are also present. Saturn has a very hot interior, reaching 12,000 Kelvin (11,700°C) at the core, and it radiates more energy into space than it receives from the Sun. Most of the extra energy is generated by the Kelvin-Helmholtz mechanism (slow gravitational compression), but this alone may not be sufficient to explain Saturn's heat production. An additional proposed mechanism by which Saturn may generate some of its heat is the "raining out" of droplets of helium deep in Saturn's interior, the droplets of helium releasing heat by friction as they fall down through the lighter hydrogen.

Saturn's atmosphere exhibits a banded pattern similar to Jupiter's (in fact, the nomenclature is the same), but Saturn's bands are much fainter and are also much wider near the equator. Saturn's winds are among the Solar System's fastes
Saturn's interior is similar to Jupiter's, having a rocky core at the center, a liquid metallic hydrogen layer above that, and a molecular hydrogen layer above that. Traces of various ices are also present. Saturn has a very hot interior, reaching 12,000 Kelvin (11,700°C) at the core, and it radiates more energy into space than it receives from the Sun. Most of the extra energy is generated by the Kelvin-Helmholtz mechanism (slow gravitational compression), but this alone may not be sufficient to explain Saturn's heat production. An additional proposed mechanism by which Saturn may generate some of its heat is the "raining out" of droplets of helium deep in Saturn's interior, the droplets of helium releasing heat by friction as they fall down through the lighter hydrogen.

Semi-major axis 1,426,725,413 km
9.537 070 32 AU
Orbital circumference 8.958 Tm
59.879 AU
Eccentricity 0.054 150 60
Perihelion 1,349,467,375 km
9.020 632 24 AU
Aphelion 1,503,983,449 km
10.053 508 40 AU
Orbital period 10,756.1995 d
(29.45 a)
Synodic period 378.10 d
Avg. orbital speed 9.639 km/s
Max. orbital speed 10.183 km/s
Min. orbital speed 9.137 km/s
Inclination 2.484 46°
(5.51° to Sun's equator)
Longitude of the
ascending node 113.715 04°
Argument of the
perihelion 338.716 90°
Number of satellites 56 confirmed [17]

Saturn's atmosphere exhibits a banded pattern similar to Jupiter's (in fact, the nomenclature is the same), but Saturn's bands are much fainter and are also much wider near the equator. Saturn's winds are among the Solar System's fastest; Voyager data indicates peak easterly winds of 500 m/s (1116 mph)[3]. Saturn's finer cloud patterns were not observed until the Voyager flybys. Since then, however, Earth-based telescopy has improved to the point where regular observations can be made.

Saturn's usually bland atmosphere occasionally exhibits long-lived ovals and other features common on Jupiter; in 1990 the Hubble Space Telescope observed an enormous white cloud near Saturn's equator which was not present during the Voyager encounters and in 1994 another, smaller storm was observed. The 1990 storm was an example of a Great White Spot, a unique but short-lived Saturnian phenomenon with a roughly 30-year periodicity. Previous Great White Spots were observed in 1876, 1903, 1933, and 1960, with the 1933 storm being the most famous. The careful study of these episodes reveals interesting patterns; if it holds another storm will occur in about 2020.(Kidger 1992)

Recent images from the Cassini spacecraft show that Saturn's northern hemisphere is changing colors. It now appears a bright blue, similar to Uranus, as can be seen in the image below. This blue color cannot currently be observed from earth, because Saturn's rings are currently blocking its northern hemisphere. One theory is that this shocking color change is a result of colder temperatures, as the shadows cast by Saturn's rings are blocking out sunlight. This would result in the yellow clouds sinking and Saturn's deeper blue atmosphere being revealed

Answer 5

saturn is the most beautifull object seen from space

Answer 6

An automobile company that started in 1982.

Answer 7

saturn is the 6th planet

Answer 8

Saturn-

The second-largest planet in the solar system and the sixth in order of distance to the Sun. The outermost planet known prior to 1781, Saturn is surrounded by a beautiful system of rings. Saturn is also the only planet that has a satellite (Titan) with a dense atmosphere. This distant planetary system has been visited by four NASA spacecraft, including Cassini, which went into orbit around the planet in July 2004.

Saturn makes one revolution about the Sun in 29.42 years. The equatorial diameter of Saturn is about 75,000 mi (120,540 km), and the polar diameter about 67,600 mi (108,700 km). The volume is 769 (Earth = 1) with a few percent uncertainty. The mass is about 95.2 (Earth = 1) or 1/3500 (Sun = 1). The mean density is 0.70 g/cm3, the lowest mean density of all the planets. The rotation axis of both the planet and the rings is inclined 27° to the perpendicular to the orbital plane. The visible cloud layers of Saturn are much more homogeneous than those of Jupiter. There is no feature comparable to the Great Red Spot, and the contrast of the features that are visible is very low.

Saturn, viewed from Voyager 1. The soft, velvety appearance of the low-contrast banded structure is due to scattering by a haze layer above the planet's cloud deck. (NASA)

The optical spectrum of Saturn is characterized by strong absorption bands of methane (CH4) and by much weaker bands of ammonia (NH3). Absorption lines of molecular hydrogen (H2) have also been detected.

The temperature the planet should assume in response to solar heating is calculated to be about 76 K (?323°F), somewhat lower than the measured value of 92 K (?294°F). This suggests that Saturn has an internal heat source of roughly the same magnitude as that on Jupiter. As in the case of Jupiter, a thermal inversion exists in the upper atmosphere. The inversion region is well above the main cloud layer, which is thought to consist primarily of frozen ammonia crystals, with an admixture of some other substances to provide the yellowish color sometimes observed in the equatorial zone.

Theoretical models for the internal structure of Saturn are similar to those for Jupiter, that is, a dense core surrounded by hydrogen compressed to a metallic state which gradually merges into an extremely deep atmosphere. The fact that the two planets radiate comparable amounts of energy despite their difference in size means that smaller Saturn must have some additional energy source besides gravitational contraction. The existence of a magnetic field and belts of trapped electrons has been deduced from observations of nonthermal radiation and mapped out in detail by the Pioneer and Voyager spacecraft.

Jupiter and Saturn are relatively similar bodies. Both seem to have compositions virtually identical with that of the Sun and the other stars—rich in hydrogen and helium. In that sense, they may represent the primitive material from which the entire solar system was formed, whereas the other planets have undergone fractionation processes resulting in the loss of most of the light gases. This conclusion has been strengthened by measurements of the heavy isotope of hydrogen known as deuterium. They demonstrate that the hydrogen that makes up most of the mass of both Jupiter and Saturn was captured directly from the solar nebula when these planets formed 4.5 billion years ago. However, both Jupiter and Saturn show an enhancement of the carbon/hydrogen ratio (as determined from methane and hydrogen) compared with the Sun. This suggests that both of these planets formed in a two-stage process that led initially to formation of a large core with an outgassed, secondary atmosphere, followed by the attraction of an envelope of gases from the surrounding nebula. See also Planetary physics.

The most remarkable feature associated with Saturn is the complex ring system that surrounds the planet (Fig. 2). The system is divided into four main regions, designated A through D. The narrow F ring is located just beyond the edge of ring A, and there are G and E rings still farther out. Each of the four main regions is subdivided into many individual “ringlets,” so that Saturn is actually surrounded by thousands of rings. The ring system is made up of myriad separate particles that move independently in flat, mostly circular orbits in Saturn's equatorial plane. Periodic perturbations by the major satellites are responsible, in part, for the main divisions of Saturn's rings.

Saturn's rings, viewed from Voyager 1. Approximately 95 individual concentric features are visible. One of the satellites discovered by Voyager 1 is visible just inside the narrow F ring. (NASA)

As of July 2004, Saturn had 30 confirmed satellites. The largest and brightest, Titan, is visible with small telescopes; the other satellites are much fainter. Titan's mean apparent diameter corresponds to a linear diameter of approximately 3440 mi (5550 km). But this diameter refers to the satellite's atmosphere, which is filled with a dense aerosol produced photochemically by incident sunlight. The solid surface of Titan has a diameter of 3200 mi (5150 km), making this satellite larger than Mercury but smaller than Jupiter's giant Ganymede. This object contains a large fraction of icy material and is thus quite different from the Moon or the inner planets in composition. Furthermore, it is large and cold enough to retain a thick, nitrogen (N2)-dominated atmosphere that contains a few percent of methane (CH4) and exerts a surface pressure of 1.5 bars (1.5 × 105 Pa), or 1.5 times the sea-level pressure on Earth. The main constituent of this atmosphere is molecular nitrogen. The surface of Titan is so cold [94 ± 2K or (?290 ± 4°F] that takes of liquid ethane may be present..

Answer 9

All the info you need is at http://www.nasa.gov/ all you have to do is do a search on saturn.

Answer 10

That's what wikipedia is for