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Enceladus - Wikipedia. Enceladus (; en- SEL- . It is about 5. 00 kilometers (3.

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Enceladus is mostly covered by fresh, clean ice, making it one of the most reflective bodies of the solar system. Consequently, its surface temperature at noon only reaches . Despite its small size, Enceladus has a wide range of surface features, ranging from old, heavily cratered regions to young, tectonically deformed terrains that formed as recently as 1. Enceladus was discovered on August 2.

In honour of Apollo 11, here are 11 strange facts you didn’t know about the first Moon landing. Enceladus (/ . It is about 500 kilometers (310 mi) in diameter, about a tenth of that.

William Herschel. In particular, Cassini discovered water- rich plumes venting from the south polar region. Like many other satellites in the extensive systems of the giant planets, Enceladus is trapped in an orbital resonance. Its resonance with Dione excites its orbital eccentricity, which is damped by tidal forces, tidally heating its interior, and possibly driving the geological activity. History. Like many satellites of Saturn discovered prior to the Space Age, Enceladus was first observed during a Saturnian equinox, when Earth is within the ring plane. At such times, the reduction in glare from the rings makes the moons easier to observe. Only its orbital characteristics were known, with estimations of its mass, density and albedo.

Enceladus is named after the giant. Enceladus of Greek mythology. The IAU has officially named 8. Enceladus, most recently Samaria Rupes, formerly called Samaria Fossa. It orbits at 2. 38,0. Saturn's center and 1.

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Mimas and Tethys. It orbits Saturn every 3. Enceladus is currently in a 2: 1 mean- motion orbital resonance with Dione, completing two orbits around Saturn for every one orbit completed by Dione. This resonance maintains Enceladus's orbital eccentricity (0. This non- zero eccentricity results in tidal deformation of Enceladus. The dissipated heat resulting from this deformation is the main heating source for Enceladus's geologic activity. Unlike Earth's Moon, Enceladus does not appear to librate about its spin axis (more than 1.

However, analysis of the shape of Enceladus suggests that at some point it was in a 1: 4 forced secondary spin–orbit libration. It is an extremely wide but diffuse disk of microscopic icy or dusty material distributed between the orbits of Mimas and Titan. In the 1. 98. 0s some suspected that Enceladus is the main source of particles for the ring. Examination of the resulting highest- resolution imagery revealed at least five different types of terrain, including several regions of cratered terrain, regions of smooth (young) terrain, and lanes of ridged terrain often bordering the smooth areas.

Given the relative lack of craters on the smooth plains, these regions are probably less than a few hundred million years old. Accordingly, Enceladus must have been recently active with . The smooth plains, which Voyager 2 had observed, resolved into relatively crater- free regions filled with numerous small ridges and scarps. Numerous fractures were found within the older, cratered terrain, suggesting that the surface has been subjected to extensive deformation since the craters were formed. There are fissures, plains, corrugated terrain and other crustal deformations. Several additional regions of young terrain were discovered in areas not well- imaged by either Voyager spacecraft, such as the bizarre terrain near the south pole.

Much of Enceladus' surface is covered with craters at various densities and levels of degradation. The rate at which this occurs is dependent on the temperature of the ice: warmer ice is easier to deform than colder, stiffer ice. Viscously relaxed craters tend to have domed floors, or are recognized as craters only by a raised, circular rim. Dunyazad crater is a prime example of a viscously relaxed crater on Enceladus, with a prominent domed floor. These canyons can be up to 2. Such features are geologically young, because they cut across other tectonic features and have sharp topographic relief with prominent outcrops along the cliff faces. These bands, first discovered by Voyager 2, often separate smooth plains from cratered regions.

However, unlike those seen on Ganymede, grooved topography on Enceladus is generally more complex. Rather than parallel sets of grooves, these lanes often appear as bands of crudely aligned, chevron- shaped features. In other areas, these bands bow upwards with fractures and ridges running the length of the feature.

Cassini observations of the Samarkand Sulci have revealed dark spots (1. Currently, these spots are interpreted as collapse pits within these ridged plain belts.

Many of these fractures are found in bands cutting across cratered terrain. These fractures probably propagate down only a few hundred meters into the crust. Many have probably been influenced during their formation by the weakened regolith produced by impact craters, often changing the strike of the propagating fracture.

These linear grooves can be seen cutting across other terrain types, like the groove and ridge belts. Like the deep rifts, they are among the youngest features on Enceladus. However, some linear grooves have been softened like the craters nearby, suggesting that they are older. Ridges have also been observed on Enceladus, though not nearly to the extent as those seen on Europa. These ridges are relatively limited in extent and are up to one kilometer tall. One- kilometer high domes have also been observed. They generally have low relief and have far fewer craters than in the cratered terrains, indicating a relatively young surface age.

Another region of smooth plains to the southwest of Sarandib is criss- crossed by several troughs and scarps. Cassini has since viewed these smooth plains regions, like Sarandib Planitia and Diyar Planitia at much higher resolution. Cassini images show these regions filled with low- relief ridges and fractures, probably caused by shear deformation. Download Whole Strange Magic (2015) Movie.

Rather than being covered in low- relief ridges, this region is covered in numerous criss- crossing sets of troughs and ridges, similar to the deformation seen in the south polar region. This area is on the opposite side of Enceladus from Sarandib and Diyar Planitiae, suggesting that the placement of these regions is influenced by Saturn's tides on Enceladus. This area, reaching as far north as 6. They appear to be the youngest features in this region and are surrounded by mint- green- colored (in false color, UV–green–near IR images), coarse- grained water ice, seen elsewhere on the surface within outcrops and fracture walls. Results from the visual and infrared spectrometer (VIMS) instrument suggest that the green- colored material surrounding the tiger stripes is chemically distinct from the rest of the surface of Enceladus. VIMS detected crystalline water ice in the stripes, suggesting that they are quite young (likely less than 1,0. The shape, orientation, and location of these features suggest they are caused by changes in the overall shape of Enceladus.

As of 2. 00. 6 there were two theories for what could cause such a shift in shape: the orbit of Enceladus may have migrated inward, leading to an increase in Enceladus's rotation rate. Such a shift would lead to a more oblate shape.

One problem of the polar flattening hypothesis is that both polar regions should have similar tectonic deformation histories. Variations in lithospheric thickness are supported by the correlation between the Y- shaped discontinuities and the V- shaped cusps along the south polar terrain margin and the relative surface age of the adjacent non- south polar terrain regions. The Y- shaped discontinuities, and the north- south trending tension fractures into which they lead, are correlated with younger terrain with presumably thinner lithospheres. The V- shaped cusps are adjacent to older, more heavily cratered terrains. However, flybys by Cassini provided information for models of Enceladus's interior, including a better determination of the mass and shape, high- resolution observations of the surface, and new insights on the interior.