Abstract
Results from radar observations of Mercury are reviewed, the used as a basis for comparison of Mercury with its closest geologic relative, the Moon. Both bodies show very similar quasispecular scattering properties, indicating surfaces which are, on average, rougher (on scales of meters) and more porous than those of Venus and Mars. As with the Moon, some of the more prominent radar features on Mercury are associated with fresh, rayed craters. Mercury also has some prominent radar-bright features in the unimaged hemisphere which show no obvious impact structure; these features may come from smooth plains and possibly even (in one case) a large shield volcano. The Mercurian smooth plains show the quasispecular smoothness and down-bowed topography characteristic of lunar maria, providing support for the idea that the smooth plains and maria are geologic analogues. Permanently shaded craters at the north and south poles of Mercury show extremely bright radar features consistent with volume scattering from ice deposits. This discovery has helped to revive the old idea that ice may exist at the lunar poles. Recent radar searches for this lunar ice have proved either negative or inconclusive.
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