1. Discovery

2. Origins

3. See also

4. References

Saturn's moon Iapetus has a long, 20-kilometer-high ridge running along most of its equator. It was discovered by the Cassini probe in 2004. The ridge's origin is unknown. There are bright areas on the sides of the equatorial ridge near Iapetus' bright trailing hemisphere, which were already visible in Voyager images appearing like mountains and were nicknamed the "Voyager Mountains".^[1]

Discovery

Iapetus's equatorial ridge was discovered when the Cassini spacecraft imaged Iapetus on 31 December 2004. Peaks in the ridge rise more than 20 km above the surrounding plains, making them some of the tallest mountains in the Solar System. The ridge forms a complex system including isolated peaks, segments of more than 200 km and sections with three near parallel ridges.^[2]

Origins

Within the bright regions there is no ridge, but there are a series of isolated 10 km peaks along the equator.^[3] The ridge system is heavily cratered, indicating that it is ancient. The prominent equatorial bulge gives Iapetus a walnut-like appearance.

It is not clear how the ridge formed. One difficulty is to explain why it follows the equator almost perfectly. There are at least four current hypotheses, but none of them explains why the ridge is confined to Cassini Regio.

• A team of scientists associated with the Cassini mission have argued that the ridge could be a remnant of the oblate shape of the young Iapetus, when it was rotating more rapidly than it does today.^[4] The height of the ridge suggests a maximum rotational period of 17 hours. If Iapetus cooled fast enough to preserve the ridge but remained plastic long enough for the tides raised by Saturn to have slowed the rotation to its current tidally locked 79 days, Iapetus must have been heated by the radioactive decay of aluminium-26. This isotope appears to have been abundant in the solar nebula from which Saturn formed, but has since all decayed. The quantities of aluminium-26 needed to heat Iapetus to the required temperature give a tentative date to its formation relative to the rest of the Solar System: Iapetus must have come together earlier than expected, only two million years after the asteroids started to form.
• The ridge could be icy material that welled up from beneath the surface and then solidified. If it had formed away from the position of the equator at the time, this hypothesis requires that the rotational axis would have been driven to its current position by the ridge.{{Citation needed|date=September 2007}}
• Iapetus may have had a ring system during its formation due to its large Hill sphere, and the equatorial ridge could have then been produced by collisional accretion of this ring.^[5]
• The ridge and the bulge could be the result of ancient convective overturn. This hypothesis states that the bulge is in isostatic equilibrium typical for terrestrial mountains. It means that under the bulge there is material of low density (roots). The weight of the bulge is compensated by buoyancy forces acting on the roots. The ridge is also built of less dense matter. Its position along the equator is probably a result of the Coriolis force acting on a liquid interior of Iapetus.^[6][7]

See also

• Subsatellite

References

• INF-γ
• INF-γ receptor
• ING1
• ING2
• ING3
• Ing 3 (disambiguation)
• ING4
• ING5
• IN-GA
• Inga Aaberg
• Inga Aberg
• Inga Afonina
• Inga and Anush Arshakyan
• Inga & Anush Arshakyan
• Inga Arshakyan
• Inga Artomonova
• Inga atropicta
• Inga Babakhova
• Inga Balstad
• Inga Benedict-Thompson
• Inga Bergstorm
• Inga Berit Svestad
• Inga bigemina
• Inga Bjork-Klevby
• Inga Björk-Klevby