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Miranda (moon)

PIA18185 Miranda's Icy Face.jpg
Discovered by Gerard P. Kuiper
Discovery date February 16, 1948
Pronunciation /mɪˈrændə/ mi-RAN-də
Uranus V
Adjectives Mirandan, Mirandian
Orbital characteristics
129390 km
Eccentricity 0.0013
1.413479 d
6.66 km/s (calculated)
Inclination 4.232° (to Uranus's equator)
Satellite of Uranus
Physical characteristics
Dimensions 480 × 468.4 × 465.8 km
Mean radius
235.8±0.7 km (0.03697 Earths)[1]
700000 km2
Volume 54835000 km3

(6.59±0.75)×1019 kg[2]

(1.103×10−5 Earths)
Mean density
1.20±0.15 g/cm3[2]
0.079 m/s2
0.193 km/s
Albedo 0.32
Surface temp. min mean max
solstice[3] ? ≈ 60 K 84±1 K

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, and named after Miranda from William Shakespeare's play The Tempest.[5] 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's extreme seasonal cycle.

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. There are no active plans at present to return to study the moon in more detail, although various concepts such as a Uranus orbiter and probe have been proposed from time to time.

Like all of Uranus' moons, 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 5- to 10-kilometer-high scarp, 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.

Discovery and name

Miranda was discovered on 16 February 1948 by planetary astronomer Gerard Kuiper using the McDonald Observatory's 82-inch (2,080 mm) Otto Struve Telescope.[5][6] Its motion around Uranus was confirmed on 1 March 1948.[5] It was the first satellite of Uranus discovered in nearly 100 years. Kuiper elected to name the object "Miranda" after the character in Shakespeare's The Tempest, because the four previously discovered moons of Uranus, Ariel, Umbriel, Titania and Oberon, had all been named after characters of Shakespeare or Alexander Pope. However, the previous moons had been named specifically after fairies,[7] whereas Miranda was a human. Subsequently, discovered satellites of Uranus were named after characters from Shakespeare and Pope, whether fairies or not.


Of Uranus's five round satellites, Miranda orbits closest to it, at roughly 129,000 km from the surface; about a quarter again as far as its most distant ring. Its orbital period is 34 hours, and, like that of the Moon, is synchronous with its rotation period, which means it always shows the same face to Uranus, a condition known as tidal lock. Miranda's orbital inclination (4.34°) is unusually high for a body so close to its planet, and roughly ten times that of the other major Uranian satellites. The reason for this is still uncertain; there are no mean-motion resonances between the moons that could explain it, leading to the hypothesis that the moons occasionally pass through secondary resonances, which at some point in the past led to Miranda being locked for a time into a 3:1 resonance with Umbriel, before chaotic behaviour induced by the secondary resonances moved it out of it again.[8] In the Uranian system, due to the planet's lesser degree of oblateness, and the larger relative size of its satellites, escape from a mean-motion resonance is much easier than for satellites of Jupiter or Saturn.[9][10]

Physical characteristics

Close-up of Verona Rupes, a large fault scarp on Miranda possibly 5 km (3.1 mi) high,[11][12] taken by Voyager 2 in January 1986

At 1.2 g/cm3, Miranda is the least dense of Uranus's round satellites. That density suggests a composition of more than 60% water ice.[13] Miranda's surface may be mostly water ice, with the low-density body also probably containing silicate rock and organic compounds in its interior.

Miranda's surface has patchwork regions of broken terrain indicating intense geological activity in Miranda's past, and is criss-crossed by huge canyons. It also has the largest known cliff in the Solar System, Verona Rupes, which has a height of over 5 km (3.1 mi). Some of Miranda's terrain is possibly less than 100 million years old based on crater counts, which suggests that Miranda may still be geologically active today.[14]

There are three giant 'racetrack'-like grooved structures called coronae in the southern hemisphere, each at least 200 km (120 mi) wide and up to 20 km (12 mi) deep, named Arden, Elsinore and Inverness after locations in Shakespeare's plays, may have formed via extensional processes at the tops of diapirs, or upwellings of warm ice.[12][15][16][17] It is believed through computer modelling that Miranda may have an additional corona on the unimaged hemisphere.[18]

The ridges probably represent extensional tilt blocks. The canyons probably represent graben formed by extensional faulting. Other features may be due to cryovolcanic eruptions of icy magma. The diapirs may have changed the density distribution within Miranda, which could have caused Miranda to reorient itself,[19] similar to a process believed to have occurred at Saturn's geologically active moon Enceladus.

Miranda's past geological activity is believed to have been driven by tidal heating during the time when it was in orbital resonance with Umbriel.[20] The resonance would have increased orbital eccentricity; resulting tidal friction due to time-varying tidal forces from Uranus would have caused warming of Miranda's interior.[9][10]

Miranda may have also once been in a 5:3 resonance with Ariel, which would have also contributed to its internal heating. However, the maximum heating attributable to the resonance with Umbriel was likely about three times greater.[20]

An earlier theory, proposed shortly after the Voyager 2 flyby, was that a previous incarnation of Miranda was shattered by a massive impact, with the fragments reassembling and denser ones subsequently sinking to produce the current strange pattern.[12]

Approaching the 7 December 2007 equinox Miranda produced brief solar eclipses over the center of Uranus.

Scientists recognize the following geological features on Miranda:

Observation and exploration

A computer-simulated flight over Miranda

Miranda's apparent magnitude is +16.6, making it invisible to many amateur telescopes.[21] Virtually all known information regarding its geology and geography was obtained during the flyby of Uranus made by Voyager 2 in 1986, The closest approach of Voyager 2 to Miranda was 29,000 km (18,000 mi)—significantly less than the distances to all other Uranian moons.[22]

See also


  1. ^ Thomas, P. C. (1988). "Radii, shapes, and topography of the satellites of Uranus from limb coordinates". Icarus. 73 (3): 427–441. Bibcode:1988Icar...73..427T. doi:10.1016/0019-1035(88)90054-1. 
  2. ^ a b Jacobson, R. A.; Campbell, J. K.; Taylor, A. H.; Synnott, S. P. (June 1992). "The masses of Uranus and its major satellites from Voyager tracking data and earth-based Uranian satellite data". The Astronomical Journal. 103 (6): 2068–2078. Bibcode:1992AJ....103.2068J. doi:10.1086/116211. 
  3. ^ Hanel, R.; Conrath, B.; Flasar, F. M.; Kunde, V.; Maguire, W.; Pearl, J.; Pirraglia, J.; Samuelson, R.; Cruikshank, D. (4 July 1986). "Infrared Observations of the Uranian System". Science. 233 (4759): 70–74. Bibcode:1986Sci...233...70H. doi:10.1126/science.233.4759.70. PMID 17812891. 
  4. ^ "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). 2009-04-03. Retrieved 2009-08-10. 
  5. ^ a b c Kuiper, G. P., The Fifth Satellite of Uranus, Publications of the Astronomical Society of the Pacific, Vol. 61, No. 360, p. 129, June 1949
  6. ^ "Otto Struve Telescope". MacDonald Observatory. 2014. Retrieved 2014-10-21. 
  7. ^ S G Barton. "The Names of the Satellites". Popular Astronomy. 54: 122. 
  8. ^ Michele Moons and Jacques Henrard (June 1994). "Surfaces of Section in the Miranda-Umbriel 3:1 Inclination Problem". Celestial Mechanics and Dynamical Astronomy. 59 (2): 129–148. Bibcode:1994CeMDA..59..129M. doi:10.1007/bf00692129. 
  9. ^ a b Tittemore, William C.; Wisdom, Jack (March 1989). "Tidal evolution of the Uranian satellites: II. An explanation of the anomalously high orbital inclination of Miranda". Icarus. 78 (1): 63–89. Bibcode:1989Icar...78...63T. doi:10.1016/0019-1035(89)90070-5. 
  10. ^ a b Malhotra, Renu; Dermott, Stanley F. (June 1990). "The role of secondary resonances in the orbital history of Miranda". Icarus. 85 (2): 444–480. Bibcode:1990Icar...85..444M. doi:10.1016/0019-1035(90)90126-T. ISSN 0019-1035. 
  11. ^ "PIA00044: Miranda high resolution of large fault". JPL, NASA. Retrieved 2007-07-23. 
  12. ^ a b c Chaikin, Andrew (2001-10-16). "Birth of Uranus' Provocative Moon Still Puzzles Scientists". Imaginova Corp. Archived from the original on 2008-07-09. Retrieved 2007-12-07. 
  13. ^ B. A. Smith; et al. (4 July 1986). "Voyager 2 in the Uranian System: Imaging Science Results". Science. 233: 55. Bibcode:1986Sci...233...43S. doi:10.1126/science.233.4759.43. PMID 17812889. 
  14. ^ S. J. Desch; J. C. Cook; W. Hawley & T. C. Doggett (2007-01-09). "Cryovolcanism on Charon and other Kuiper Belt Objects" (PDF). Lunar and Planetary Science. XXXVIII. Retrieved 2017-08-28. 
  15. ^ Pappalardo, Robert T.; Reynolds, Stephen J.; Greeley, Ronald (1997-06-25). "Extensional tilt blocks on Miranda: Evidence for an upwelling origin of Arden Corona". Journal of Geophysical Research. 102 (E6): 13,369–13,380. Bibcode:1997JGR...10213369P. doi:10.1029/97JE00802. 
  16. ^ "Bizarre Shape of Uranus' 'Frankenstein' Moon Explained". Retrieved 2017-08-28. 
  17. ^ "Uranus Miranda - Teach Astronomy". Archived from the original on 2014-10-15. Retrieved 2017-08-28. 
  18. ^ Choi, Charles Q. "Bizarre Shape of Uranus' 'Frankenstein' Moon Explained". Retrieved 2015-11-27. 
  19. ^ Pappalardo, Robert T.; Greeley, Ronald (1993). "Structural evidence for reorientation of Miranda about a paleo-pole". In Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z. pp. 1111–1112. Bibcode:1993LPI....24.1111P. 
  20. ^ a b Tittemore, William C.; Wisdom, Jack (June 1990). "Tidal evolution of the Uranian satellites: III. Evolution through the Miranda-Umbriel 3:1, Miranda-Ariel 5:3, and Ariel-Umbriel 2:1 mean-motion commensurabilities". Icarus. 85 (2): 394–443. Bibcode:1990Icar...85..394T. doi:10.1016/0019-1035(90)90125-S. 
  21. ^ Doug Scobel (2005). "Observe the Outer Planets!". The University of Michigan. Retrieved 2014-10-24. 
  22. ^ Stone, E. C. (December 30, 1987). "The Voyager 2 Encounter with Uranus". Journal of Geophysical Research. 92 (A13): 14,873–14,876. Bibcode:1987JGR....9214873S. doi:10.1029/JA092iA13p14873. 

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