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Iapetus (moon)

Discovered byGiovanni Cassini
Discovered in1671
Orbital characteristics
Semimajor axis3,561,300 km
Revolution period79d 7h 55m
Is a satellite ofSaturn
Physical characteristics
Mean radius718 km
Surface area6,700,000 km2
Mass1.9739×1021 kg
Mean density1.27 g/cm3
Surface gravity? m/s2
Rotation period79d 7h 55m (synchronous)
Axial tilt14.84°

Iapetus is the third-largest moon of Saturn, discovered by Giovanni Cassini in 1671.

Its density is similar to that of Rhea, indicating that it has a small amount of rocky materials. Its leading side is dark (albedo 0.03-0.05) with a slight reddish color while its trailing side is bright (albedo 0.5, almost as bright as Europa). This difference is so striking that Cassini noted that he could see Iapetus only on one side of Saturn and not on the other. The dark surface might be composed of matter that was either swept up from space or oozed from the moon's interior; the real source is still unknown. The dark material might be a thin layer of organic material perhaps similar to the complex substances found in the most primitive meteorites. However, there are no bright-rimed craters present on the dark hemisphere; If the dark material is thin, it must be constantly renewed since a meteor impact would punch through the layer to reveal brighter surface material.

The dark material may have originated from Phoebe, which has a very low albedo. Micrometeor impacts could kick dark matter off Phoebe which is then swept up by Iapetus (Phoebe, however, has a slightly different color from that of the dark surface of Iapetus.) The fact that the material is on the leading hemisphere seems to support this theory. On the other hand, the dark material seems to be concentrated in crater floors. This would indicate an internal origin. Since Iapetus is so far from Saturn and thus avoided much of the heating its other moons received, it may have formed with methane or ammonia ice in its interior; the dark material could be explained by volcano-like eruptions of methane. This theory is supported by a dark ring of material about 100 kilometers in diameter that straddles the border between the leading and trailing hemispheres of Iapetus. Such rings formed on the Moon and on Mars when dark volcanic material flowed into impact craters and filled around the central peak.

Iapetus is one of only two major Saturnian moons to have a significantly inclined orbital plane (the other is Phoebe).

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