Equatorial ridge on Iapetus

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.{{cite journal| last=Porco | first=C. C. | author-link = Carolyn Porco | author2=E. Baker, J. Barbara, K. Beurle, A. Brahic, J. A. Burns, S. Charnoz, N. Cooper, D. D. Dawson, A. D. Del Genio, T. Denk, L. Dones, U. Dyudina, M. W. Evans, B. Giese, K. Grazier, P. Helfenstein, A. P. Ingersoll, R. A. Jacobson, T. V. Johnson, A. McEwen, C. D. Murray, G. Neukum, W. M. Owen, J. Perry, T. Roatsch, J. Spitale, S. Squyres, P. C. Thomas, M. Tiscareno, E. Turtle, A. R. Vasavada, J. Veverka, R. Wagner, R. West| date=2005-02-25 ==Origins==

Within the bright regions there is no ridge, but there are a series of isolated 10 km peaks along the equator. 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. 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. • 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. • Iapetus could have been impacted by a body that created both a ring system and a subsatellite, which would be possible due to the large Hill sphere mentioned above. The subsatellite then proceeds to quickly force the ring system down onto Iapetus, creating the ridge system, before escaping Iapetus' gravity via tidal acceleration. • 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. == Gallery ==

File:Iapetus_Voyager2_flyby_sequence.jpg|This series of images of Iapetus' north pole by Voyager 2 became the first-ever hints on the existence of the moon's equatorial ridge. The white and grey dots below each images (Iapetus' equator) will later be revealed to be Carcassone Montes Taken on August 22, 1981. File:Iapetus.jpg|A global view of Iapetus obtained by the Cassini spacecraft on Dec. 31, 2004 - the first-ever clear image of the ridge - at a distance of about 172,900 kilometers (107,435 miles). The massive structure clearly distorts the shape of the moon at the equator. File:Iapetus_crescent_true_color.png|Iapetus' massive equatorial ridge is clearly visible from ''Cassini's'' images as the space probe approached Iapetus from its nightside during its closest flyby of the moon on September 10, 2007 at a distance of 83,000 kilometers (51,600 miles). The spacecraft came as close as from the moon's surface during this flyby. This is also the clearest picture of the equatorial ridge to date. ==See also==