Miranda (moon)

Miranda, also designated Uranus V, is the smallest and innermost of Uranus's five round satellites. It was discovered by Gerard Kuiper on 16 February 1948 at McDonald Observatory in Texas, and named after Miranda from William Shakespeare's play The Tempest.[10] Like the other large moons of Uranus, Miranda orbits close to its planet's equatorial plane. Because Uranus orbits the Sun on its side, Miranda's orbit is perpendicular to the ecliptic and shares Uranus' extreme seasonal cycle.

Miranda
Discovery
Discovered byGerard P. Kuiper
Discovery dateFebruary 16, 1948
Designations
Designation
Uranus V
Pronunciation/mɪˈrændə/[1][2]
AdjectivesMirandan,[3] Mirandian[4]
Orbital characteristics
129,390 km
Eccentricity0.0013
1.413479 d
6.66 km/s (calculated)
Inclination4.232° (to Uranus's equator)
Satellite ofUranus
Physical characteristics
Dimensions480×468.4×465.8 km
Mean radius
235.8±0.7 km (0.03697 Earths)[5]
700,000 km2
Volume54,835,000 km3
Mass(6.4±0.3)×1019 kg[6]
Mean density
1.20±0.15 g/cm3[7]
0.079 m/s2
0.193 km/s
synchronous
Albedo0.32
Surface temp. min mean max
solstice[8] ? 60 K 84±1 K
15.8[9]

At just 470 km in diameter, Miranda is one of the smallest closely observed objects in the Solar System that might be in hydrostatic equilibrium (spherical under its own gravity). The only close-up images of Miranda are from the Voyager 2 probe, which made observations of Miranda during its Uranus flyby in January 1986. During the flyby, Miranda's southern hemisphere pointed towards the Sun, so only that part was studied.

Miranda probably formed from an accretion disc that surrounded the planet shortly after its formation, and, like other large moons, it is likely differentiated, with an inner core of rock surrounded by a mantle of ice. Miranda has one of the most extreme and varied topographies of any object in the Solar System, including Verona Rupes, a 20-kilometer-high scarp that is the highest cliff in the Solar System,[11][12] and chevron-shaped tectonic features called coronae. The origin and evolution of this varied geology, the most of any Uranian satellite, are still not fully understood, and multiple hypotheses exist regarding Miranda's evolution.