Miranda (moon)

From Academic Kids

Missing image

Discovered by Gerard Kuiper
Discovered in 1948
Orbital characteristics
Mean radius 129,872 km
Eccentricity ~0.0013
Orbital period 1.413479d
Inclination 4.34
Is a satellite of Uranus
Physical characteristics
Mean diameter 471.6 km
Surface area km2
Mass 6.59×1019 kg
Mean density 1.20 g/cm3
Surface gravity 0.079 m/s2
Rotation period 1.413479 days
Axial tilt  ?
Albedo 0.34
Surface temp. 86 K
Atmospheric pressure 0 kPa

Miranda (mi-ran'-da) is the smallest and innermost of Uranus' major moons.

It was discovered by Gerard Kuiper on 1948-02-16 at Fort Davis. It is named after Prospero's daughter in William Shakespeare's play The Tempest. It is also designated Uranus V.

So far the only close-up images of Miranda are from the Voyager 2 probe, which made observations of the moon during its Uranus flyby in January, 1986. During the flyby the southern hemisphere of the moon was pointed towards the Sun so only it was studied. It was a fortunate coincidence that the moon passed by at the closest distance by Voyager 2 turned out to be the geologically most active body in the Uranus system.

Missing image
Close-up view of Verona Rupes, a large fault scarp on Miranda; at 12km high, it is the highest cliff in the solar system

Physical characteristics

Miranda's surface may be mostly water ice, with the low density body being made of silicate rock and methane-related organic compounds. Miranda's surface is criss-crossed by huge canyons up to 20 kilometres (12 miles) deep, with patchwork regions of broken terrain indicating intense geological activity in the moon's past. Large grooved structures, called coronae, may be the result of upwelling warm ice. It is thought that this activity is powered by tidal forces from Uranus. Another theory, now considered less likely, suggests that Miranda was at some point struck by a massive object that shattered the moon. Fragments then resettled into different positions forming the current strange pattern.

Miranda's orbital inclination (4.34°) is unusually high for a body so close to the planet. It is possible that it was at some point in a 3:1 orbital resonance with Umbriel. Resulting tidal friction may also have caused warming within the moon and thus be the culprit of the geological activity.

Scientists recognize the following geological features on Miranda:

See also

External links

Uranus' natural satellites

edit  (http://academickids.com/encyclopedia/index.php?title=Template:Uranus_Footer&action=edit)

Cordelia | Ophelia | Bianca | Cressida | Desdemona | Juliet | Portia | Rosalind | S/2003 U 2 | Belinda
S/1986 U 10 | Puck | S/2003 U 1 | Miranda | Ariel | Umbriel | Titania | Oberon | S/2001 U 3
Caliban | Stephano | Trinculo | Sycorax | S/2003 U 3 | Prospero | Setebos | S/2001 U 2
bg:Миранда (спътник)

ca:Miranda (Satllit) de:Miranda (Mond) es:Miranda (luna) fr:Miranda (lune) he:מירנדה (ירח) nl:Miranda (maan) ja:ミランダ nn:Uranusmnen Miranda ru:Миранда (спутник Урана) sk:Miranda (mesiac) zh:天卫五


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