Jump to content

Miranda (moon): Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous editNext edit →
Content deleted Content added
VisualWikitext
AnomieBOT (talk | contribs)
Bots
6,401,294 edits
Rescuing orphaned refs ("Jacobson1992" from Uranus)
m Reverted edits by AnomieBOT (talk) to last version by Rich Farmbrough
Line 21: Line 21:
| surface_area = 700&nbsp;000 [[square kilometre|km<sup>2</sup>]]
| surface_area = 700&nbsp;000 [[square kilometre|km<sup>2</sup>]]
| volume = 54&nbsp;835&nbsp;000 [[cubic kilometre|km<sup>3</sup>]]
| volume = 54&nbsp;835&nbsp;000 [[cubic kilometre|km<sup>3</sup>]]
| mass = {{nowrap|6.59 ± 0.75{{Esp|19}} [[kilogram|kg]]}}<ref name=Jacobson1992/>
| mass = {{nowrap|6.59 ± 0.75{{Esp|19}} [[kilogram|kg]]}}<ref name=Jacobson1992>{{cite journal|last=Jacobson|first=R.A.|coauthors=Campbell, J.K.; Taylor, A.H.; Synnott, S.P.|title=The masses of Uranus and its major satellites from Voyager tracking data and Earth-based Uranian satellite data|journal=The Astronomical Journal|volume=103|issue=6|pages=2068&ndash;2078|year=1992|doi=10.1086/116211| url=http://adsabs.harvard.edu/abs/1992AJ....103.2068J}}</ref>
(1.103{{Esp|&ndash;5}} Earths)
(1.103{{Esp|&ndash;5}} Earths)
| density = {{nowrap|1.20 ± 0.15 g/cm<sup>3</sup>}}<ref name=Jacobson1992/>
| density = {{nowrap|1.20 ± 0.15 g/cm<sup>3</sup>}}<ref name=Jacobson1992/>

Revision as of 03:45, 25 September 2009

Miranda
Miranda
Discovery
Discovered byGerard P. Kuiper
Discovery dateFebruary 16, 1948
Designations
Uranus V
AdjectivesMirandian
Orbital characteristics
129 390 km
Eccentricity0.0013
1.413 479 d
Inclination4.232° (to Uranus' equator)
Satellite ofUranus
Physical characteristics
Dimensions480×468.4×465.8 km
235.8 ± 0.7 km (0.03697 Earths)[1]
700 000 km2
Volume54 835 000 km3
Mass6.59 ± 0.75 kg[2] (1.103 Earths)
Mean density
1.20 ± 0.15 g/cm3[2]
0.079 m/s2
0.193 km/s
synchronous
zero
Albedo0.32
Surface temp. min mean max
Kelvin   ~59 K 86 K
15.8[3]

Miranda (Template:Pron-en[4]) is the smallest and innermost of Uranus' five major moons.

It was discovered by Gerard Kuiper on 1948-02-16 at McDonald Observatory. It was named after Miranda from William Shakespeare's play The Tempest by Kuiper in his report of the discovery.[5] The adjectival form of the name is Mirandan. 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 that part was studied. Miranda shows more evidence of past geologic activity than any of the other Uranian satellites.

Physical characteristics

File:Miranda scarp rotated.jpg
Close-up view of Verona Rupes, a large fault scarp on Miranda; possibly 5 km (3 miles) high.[6][7]

Miranda's surface may be mostly water ice, with the low density body also likely containing silicate rock and organic compounds in its interior.

Miranda's surface has patchwork regions of broken terrain indicating intense geological activity in the moon's past, and is criss-crossed by huge canyons. Large 'racetrack'-like grooved structures, called coronae, may have formed via extensional processes at the tops of diapirs, or upwellings of warm ice.[8][9] 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 the moon, which could have caused Miranda to reorient itself,[10] similar to a process believed to have occurred at Saturn's geologically active moon Enceladus. Miranda is one of the few bodies in the solar system in which the equatorial circumference is shorter than the pole-to-pole circumference, likely a consequence of the diapir activity.

Miranda's past geological activity is believed to have been driven by tidal heating at a time when its orbit was more eccentric than currently. Early in its history, Miranda was apparently captured into a 3:1 orbital resonance with Umbriel, from which it subsequently escaped.[11] The resonance would have increased orbital eccentricity; resulting tidal friction due to time-varying tidal forces from Uranus would have caused warming of the moon's interior. In the Uranus 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. Miranda's orbital inclination (4.34°) is unusually high for a body so close to the planet. Miranda probably escaped from its resonance with Umbriel via a secondary resonance, and the mechanism of this escape is believed to explain why its orbital inclination is more than 10 times those of the other large Uranian moons (see Uranus' natural satellites).[12][13]

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.[7]

Approaching the 2007-12-07 equinox Miranda produced brief solar eclipses over the center of Uranus.

Scientists recognize the following geological features on Miranda:

  • Astronomy Domine, a song by Pink Floyd, refers to Miranda as well as Oberon and Titania.
  • In Kim Stanley Robinson's Mars Trilogy the moon is visited by the characters Ann Clayborne and Zo Boone.
  • In the fictional series Sailor Moon created by Naoko Takeuchi, Miranda Castle was the palace given to Princess Uranus by Queen Serenity when she was born. In act 41 of the manga, the other solar systerm senshi call upon the powers of their castles to allow Sailor Moon to transform into her "Eternal" form.
  • In the Novel Red Dwarf Infinity Welcomes Careful Drivers Miranda is visited by Lister.
  • In the film Serenity, the titular ship visits a forgotten planet named "Miranda".
  • Into The Miranda Rift, the novella by G. David Nordley, has four astronauts spelunking the rift when a quake closes their entry point trapping them inside the moon.

See also

References

  1. ^ Cite error: The named reference Thomas1988 was invoked but never defined (see the help page).
  2. ^ a b Cite error: The named reference Jacobson1992 was invoked but never defined (see the help page).
  3. ^ "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). 2009-04-03. Retrieved 2009-08-10.
  4. ^ In US dictionary transcription, Template:USdict.
  5. ^ 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. ^ "PIA00044: Miranda high resolution of large fault". JPL, NASA. Retrieved 2007-07-23.
  7. ^ a b Chaikin, Andrew (2001-10-16). "Birth of Uranus' provocative moon still puzzles scientists". space.com. Imaginova Corp. Retrieved 2007-07-23.
  8. ^ Pappalardo, R. T. (1997-06-25). "Extensional tilt blocks on Miranda: Evidence for an upwelling origin of Arden Corona". Journal of Geophysical Research. 102 (E6). Elsevier Science: 13, 369–13, 380. doi:10.1029/97JE00802. {{cite journal}}: External link in |last= (help); Unknown parameter |coathors= ignored (help)
  9. ^ Chaikin, Andrew (2001-10-16). "Birth of Uranus' Provocative Moon Still Puzzles Scientists". Space.Com. Imaginova Corp. Retrieved 2007-12-07.
  10. ^ Pappalardo, R. (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. Retrieved 2006-08-05. {{cite conference}}: Unknown parameter |booktitle= ignored (|book-title= suggested) (help); Unknown parameter |coauthors= ignored (|author= suggested) (help)
  11. ^ Tittemore, W. C. (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). Elsevier Science: 394–443. doi:10.1016/0019-1035(90)90125-S. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  12. ^ Tittemore, W. C. (1989). "Tidal Evolution of the Uranian Satellites II. An Explanation of the Anomalously High Orbital Inclination of Miranda". Icarus. 78: 63–89. doi:10.1016/0019-1035(89)90070-5. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  13. ^ Malhotra, R., Dermott, S. F. (1990). "The Role of Secondary Resonances in the Orbital History of Miranda". Icarus. 85: 444–480. doi:10.1016/0019-1035(90)90126-T.{{cite journal}}: CS1 maint: multiple names: authors list (link)
Retrieved from "https://en.wikipedia.org/w/index.php?title=Miranda_(moon)&oldid=316058177"