Uranus’ moon Miranda, whith a mean radius of 235.8 ± 0.7 km, is the fifth largest of Uranus’ moons. Nearly everything we know about this moon was learned from the Voyager 2 encounter in 1986. During the flyby the southern hemisphere of the moon was pointed towards the Sun, so only that part was studied.
Unlike the other four main Uranian moons, Miranda’s orbit is slightly inclined.
Miranda’s surface shows intense geological activity in the moon’s past, more than any of the other Uranian satellites and consist mostly of water ice. Its interior probably contains silicate rock and organic compounds.
Miranda sports one of the strangest and most varied landscapes among extraterrestrial bodies. The moon is criss-crossed by huge canyons as deep as 20 kilometers and it has three large features known as “coronae,” which are unique among known objects in our solar system. They are lightly cratered collections of ridges and valleys, separated from the more heavily cratered (and presumably older) terrain by sharp boundaries.
The most likely scenario is that the coronae are sites of large rocky or metallic meteorite strikes which partially melted the icy subsurface and resulted in episodic periods of slushy water rising to Miranda’s surface and refreezing.
Tidal friction from Uranus would have caused the warming of the moon’s interior.