Iapetus (moon)

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Iapetus
Missing image
Iapetus_by_Voyager_2_-_enhanced.jpg
Iapetus


Click image for description
Discovery
Discovered by Giovanni Domenico Cassini
Discovered in October 25, 1671
Orbital characteristics
Semimajor axis 3,560,820 km
Eccentricity 0.0286125 [1] (http://home.gwi.net/~pluto/mpecs/ss08.htm#elements)
Revolution period 79.3215 d
Inclination 15.47 (to Saturn's equator)
Is a satellite of Saturn
Physical characteristics
Mean diameter 1436 km
Surface area 6,700,000 km2
Mass 1.9739×1021 kg
Mean density 1.27 g/cm3
Surface gravity 0.2553 m/s2
Rotation period 79.3215 d
(synchronous)
Axial tilt zero
Albedo 0.04-0.5
Atmosphere none

Iapetus (eye-ap'-i-tus, Greek Ιαπετός) (British spelling -- "Japetus") is the third-largest moon of Saturn (see: Saturn's natural satellites), discovered by Giovanni Domenico Cassini in 1671. Iapetus is best known for its dramatic 'two-tone' coloration, but recent discoveries by the Cassini-Huygens mission have revealed several other unusual physical characteristics. These mysteries are currently under investigation by scientists and new information about Iapetus is accumulating continuously.

Contents

Name

Iapetus is named after the mythological Iapetus. It is also designated Saturn VIII.

Giovanni Cassini named the four moons he discovered (Tethys, Dione, Rhea and Iapetus) Lodicea Sidera ("the stars of Louis") to honour king Louis XIV. However, astronomers fell into the habit of referring to them and Titan as Saturn I through Saturn V. Once Mimas and Enceladus were discovered, in 1789, the numbering scheme was extended to Saturn VII.

The names of all seven satellites of Saturn then known come from John Herschel (son of William Herschel, discoverer of Mimas and Enceladus) in his 1847 publication Results of Astronomical Observations made at the Cape of Good Hope ([2] (http://adsabs.harvard.edu//full/seri/MNRAS/0008//0000042.000.html)), wherein he suggested the names of the Titans, sisters and brothers of Cronos (the Greek Saturn), be used.

Orbit

The orbit of Iapetus is somewhat unusual. Although it is one of Saturn's largest moons, it orbits much farther from Saturn than the next closest major moon, Titan. It has also the most inclined orbital plane of the regular satellites; only the irregular outer satellites like Phoebe have more inclined orbits. The cause of this is unknown.

Because of this distant, inclined orbit, Iapetus is the only large moon from which the rings of Saturn would be clearly visible; from the other inner moons, the rings would be edge-on and difficult to see.

Physical characteristics

Missing image
Iapetus_by_Saturnlight.jpg
Recent Cassini image of the night hemisphere of Iapetus, illuminated by reflected light from Saturn

The low density of Iapetus indicates that it is primarily composed of ice, with only a small amount of rocky materials.

Furthermore, Iapetus is not perfectly spherical--unusual for a large moon; parts of its globe appear to be squashed flat, and its unique equatorial ridge (see below) is so high that it visibly distorts the moon's shape even when viewed from a distance. Scientists are currently unable to describe Iapetus's shape perfectly as the Cassini probe has not yet imaged its entire surface. [3] (http://www.planetary.org/news/2005/cassini_moons_0322.html)

Iapetus is a heavily cratered body, and Cassini images have revealed large impact basins in the dark region, at least three of which are over 350 km wide. The largest has a diameter over 500 km; its rim is extremely steep and includes a scarp over 15 km high.

Two-tone coloration

In the seventeenth century, Giovanni Cassini observed that he could see Iapetus only on one side of Saturn and not on the other. He drew the conclusion that one side of Iapetus was darker than the other, a conclusion confirmed by images from the Voyager and Cassini spacecraft.

The difference between the colouring of Iapetus's two hemispheres is striking. The leading hemisphere is dark (albedo .03–.05) with a slight reddish-brown coloring, while its most of the trailing hemisphere and poles is bright (albedo .5-.6, almost as bright as Europa). The pattern of coloration is analogous to a spherical ying-yang symbol. The dark region is named Cassini Regio, and the bright region Roncevaux Terra.

The origin of this dark material is not currently known, though several theories have been proposed (see below). Its thickness is also unknown; there are no bright craters present on the dark hemisphere, so if the dark material is thin it must be constantly renewed since otherwise a meteor impact would punch through the layer to reveal brighter underlying material.

When NASA's Voyager 2 flew past Iapetus on August 22, 1981 at a relatively distant 966,000 km (600,000 miles), the spacecraft's cameras could make out few details in the area of dark material, but revealed the bright side to be icy and heavily cratered. On December 31, 2004, the Cassini spacecraft photographed Cassini Regio at far a higher resolution than Voyager was able, but the mystery surrounding its origin has only deepened.

Sources from space

Missing image
Iapetus_707_1408_0.jpg
Close-up of northern pole.

The dark material might be formed of organic compounds similar to the substances found in primitive meteorites or on the surfaces of comets; Earth-based observations have shown it to be carbonaceous and it probably includes cyano- compounds such as frozen hydrogen cyanide polymers.

An alternate theory was that the dark material originated from another Saturnian moon, Phoebe. It could have been knocked free from the smaller moon's surface by micrometeor impacts and then swept up by Iapetus' leading hemisphere. However, Phoebe's surface has a different color than that of the dark material of Iapetus - indeed it was recently announced that Phoebe's composition is closer to Iapetus's bright hemisphere than its dark one. [4] (http://www.planetary.org/news/2005/cassini_moons_0322.html)

Internal sources

It is possible that the dark material may have originated from some internal source, perhaps brought to the surface by a combination of meteor impact and cryovolcanism. This theory is supported by the apparent concentration of the material on crater floors. It has been suggested that since Iapetus is far from Saturn and would have avoided much of the heating its other moons received during the formation of the Solar system, Iapetus may have retained methane or ammonia ice in its interior that later erupted to the surface as cryovolcanic lava and was then blackened by solar radiation, charged particles, and cosmic rays. A dark ring of material about 100 kilometers in diameter straddling the border between the leading and trailing hemispheres of Iapetus is suggestive of such vulcanism, resembling structures that have formed on the Moon and on Mars as a result of volcanic material flowing into impact craters with a central peak.

Missing image
Iapetus_706_1419_1.jpg
Photomosaic of Cassini images taken Dec. 31, 2004, showing the dark Cassini Regio, large craters, and the newly discovered equatorial ridge

An alternative internal source may be the evaporation of water ice. Due to its slow rotation, Iapetus has the warmest surface in the Saturnian system (130 K in the dark region) allowing the sublimation of water ice on the surface. After sublimation, the water then freezes back to the surface and re-heats until it reaches a location where it is no longer able to sublimate. The dark areas may be the result of such a process, since the material there lacks water. However, this hypothesis fails to explain why only one hemisphere is dark.

The equatorial ridge

A further mystery was discovered when the Cassini spacecraft imaged Iapetus on December 31, 2004, and revealed a ridge about 20 km wide and 13 km high extending 1300 km through the center of Cassini Regio [5] (http://ciclops.lpl.arizona.edu/view.php?id=706). Parts of the ridge rise more than 20 km over the surrounding plains. The ridge follows the moon's equator almost perfectly and is confined to Cassini Regio. Some bright mountains near the boundary of Cassini Regio that apparently belong to this ridge were seen in Voyager photos; however, the Voyagers were unable to make out any details in the dark region itself, so the extent of the ridge is only now apparent. The ridge system is heavily cratered indicating that it is ancient.[6] (http://www.planetary.org/news/2005/cassini_moons_0322.html)

The images are currently being analyzed by scientists and no firm conclusions have yet been announced about the ridge's origin. Most scientists believe that the ridge must be icy material that welled up from beneath the surface and then solidified, but this does not explain why the ridge follows the equator. Alternatively, Paulo C.C. Freire of Arecibo Observatory has proposed that the ridge and Cassini Regio were created when Iapetus grazed the outer edges of Saturn's rings in the distant past. However's Freire's theory requires Iapetus to have been later ejected to its current, distant orbit atound Saturn. [7] (http://www.universetoday.com/am/publish/iapetus_consume_saturn_ring.html)

See also: List of geological features on Iapetus

Iapetus in fiction

  • In Arthur C. Clarke's novel 2001: A Space Odyssey (1968), astronaut Dave Bowman finds an enigmatic alien monolith waiting for him on the surface of Iapetus. A vast white ellipse is on the moon's surface, with the monolith appearing as a black dot in the center. Remarkably, when the Voyager space probes arrived at Iapetus thirteen years later, they did indeed photograph an enormous, roughly circular white region with a black region within it. Clarke reports that Carl Sagan, who was on the Voyager imaging team, sent him a photo, with the note 'Thinking of you...'
  • In Kim Stanley Robinson's futuristic novel The Memory of Whiteness, Iapetus is populated by the descendants of Soviet colonists who retain a Communist political system.

External Links

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... | Hyperion | Iapetus | Kiviuq | ...


Saturn's natural satellites
Janus' group | Mimas | Enceladus | Tethys | Dione | Rhea | Titan | Hyperion | Iapetus | Inuit group | Gallic group | Norse group
bg:Япет (спътник)

cs:Japetus (měsc) da:Iapetus (mne) de:Japetus (Mond) fr:Japet (lune) ko:이아페투스 (위성) it:Giapeto (astronomia) he:יפטוס nl:Iapetus (maan) ja:イアペトゥス (衛星) pl:Japet (księżyc) ru:Япет (cпутник) zh:土卫八

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