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Enceladus (moon)
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Enceladus (moon)

Enceladus

Discovery
Discovered by William Herschel
Discovered in 1789
Orbital characteristics
Semimajor axis 238,020 km
Eccentricity 0.0045
Orbital period 32h 53m 07s
Inclination 0.02°
Satellite of Saturn
Physical characteristics
Mean diameter 498.8 km
Mass 8.6x1019 kg
Mean density 1.3 g/cm3
Surface gravity 0.079 m/s2
Escape velocity 716 km/h
Rotation period 32h 53m 07s
(synchronous)
Axial tilt
Albedo 0.99
Surface temperature
min mean max
K 70K K
Atmosphere none

Enceladus is a moon of Saturn discovered in 1789 by William Herschel. It is named after the mythological Enceladus. It is also designated Saturn II.

The name "Enceladus" and the names of all seven satellites of Saturn then known were suggested by Herschel's son John Herschel in his 1847 publication Results of Astronomical Observations made at the Cape of Good Hope. [1]

The Cassini orbiter is due to perform a flyby of Enceladus on February 17 2005.

Physical characteristics

At least five different types of terrain have been identified on Enceladus. In addition to craters there are smooth plains and extensive linear cracks and ridges. At least some of the surface is relatively young, probably less than 100 million years. This means that Enceladus must have been active very recently with some sort of "water volcanism" or other process that renews the surface. The fresh, clean ice that dominates its surface gives Enceladus the highest albedo of any body in the solar system (Visual geometric albedo of 0.99). Because it reflects so much sunlight, the mean surface temperature is only -201°C.

Enceladus is much too small to be heated by the decay of radioactive material in its interior at present. Enceladus is locked in a 1:2 orbital resonance with Dione, similar to the situation between Io and Europa, and this may provide a tidal heating mechanism; however it is probably insufficient to melt water ice. Enceladus may therefore be composed of some low-melting point material instead of pure water. There are fissures, plains, corrugated terrain and other crustal deformations that indicates the interior of the moon may be liquid today, even though it should have frozen aeons ago.

Enceladus may be the source of the material in Saturn's tenuous E ring, and since the material cannot persist in the ring for more than a few thousand years it may be due to very recent activity on Enceladus. Another possibility, though, is that the rings are maintained by high-velocity collisions between dust particles and the various moons.

Scientists officially recognise the following geological features on Enceladus:

See also: List of geological features on Enceladus.






Saturn
Mimas | Enceladus | Tethys | Dione | Rhea | Titan | Hyperion | Iapetus | Phoebe
(For other moons, see: Saturn's natural satellites)