Metis (/ˈmtɪs/; Greek: Μήτις), also known as Jupiter XVI, is the innermost known moon of Jupiter. It was discovered in 1979 in images taken by Voyager 1, and was named in 1983 after the first wife of Zeus, Metis. Additional observations made between early 1996 and September 2003 by the Galileo spacecraft allowed its surface to be imaged.

Image taken by Galileo's Solid State Imager between November 1996 and June 1997
Discovered byS. Synnott
Discovery date4 March 1979
Orbital characteristics
Periapsis127974 km[a]
Apoapsis128026 km[a]
Mean orbit radius
128000 km (1.792 RJ)[1][2]
0.294780 d (7 h, 4.5 min)[1][2]
31.501 km/s[a]
Inclination0.06° (to Jupiter's equator)[1][2]
Satellite ofJupiter
Physical characteristics
Dimensions60 × 40 × 34 km[3]
Mean radius
21.5±2.0 km[3]
≈ 5800 km2
Volume≈ 42700 km3
Mass1.2×1017 kg[4]
Mean density
3 g/cm3[4]
Temperature≈ 123 K
Metis as taken by Galileo

Metis is tidally locked to Jupiter, and its shape is strongly asymmetrical, with one of the diameters being almost twice as large as the smallest one. It is also one of the two moons known to orbit Jupiter in less than the length of Jupiter's day, the other being Adrastea. It orbits within the main ring of Jupiter, and is thought to be a major contributor of material to the rings.

Discovery and observationsEdit

Metis was discovered in 1979 by Stephen P. Synnott in images taken by the Voyager 1 probe and was provisionally designated as S/1979 J 3.[6][7] In 1983 it was officially named after the mythological Metis, a Titaness who was the first wife of Zeus (the Greek equivalent of Jupiter).[8] The photographs taken by Voyager 1 showed Metis only as a dot, and hence knowledge about Metis was very limited until the arrival of the Galileo spacecraft. Galileo imaged almost all of the surface of Metis and put constraints on its composition by 1998.[3]

Although the Juno orbiter, which arrived at Jupiter in 2016, has a camera called JunoCam, it is almost entirely focused on observations of Jupiter itself. During close observations of Jupiter, it may capture some distant images of the innermost moons Metis and Adrastea.[9]

Physical characteristicsEdit

Metis has an irregular shape and measures 60×40×34 km across, which makes it the second smallest of the four inner satellites of Jupiter.[3] Therefore, a very rough estimate of its surface area could be placed between 5,800 and 11,600 square kilometers (approx. 8,700). The bulk composition and mass of Metis are not known, but assuming that its mean density is like that of Amalthea (~0.86 g/cm3),[10] its mass can be estimated as ~3.6×1016 kg. This density would imply that it is composed of water ice with a porosity of 10–15%.[10]

The surface of Metis is heavily cratered, dark, and appears to be reddish in color. There is a substantial asymmetry between leading and trailing hemispheres: the leading hemisphere is 1.3 times brighter than the trailing one. The asymmetry is probably caused by the higher velocity and frequency of impacts on the leading hemisphere, which excavate a bright material (presumably ice) from its interior.[5]

Orbit and rotationEdit

Metis is the innermost of Jupiter's four small inner moons. It orbits Jupiter at a distance of ~128,000 km (1.79 Jupiter radii) within Jupiter's main ring. Metis's orbit has very small eccentricity (~0.0002) and inclination (~ 0.06°) relative to the equator of Jupiter.[1][2]

Due to tidal locking, Metis rotates synchronously with its orbital period, with its longest axis aligned towards Jupiter.[2][3]

Metis lies inside Jupiter's synchronous orbit radius (as does Adrastea), and as a result, tidal forces slowly cause its orbit to decay. If its density is similar to Amalthea's, Metis's orbit lies within the fluid Roche limit; however, because it has not broken up, it must lie outside its rigid Roche limit.[2]

Metis is the fastest-moving of Jupiter's moons. It orbits Jupiter at 31.5 km/s.[a]

Relationship with Jupiter's ringsEdit

Metis's orbit lies ~1000 km within the main ring of Jupiter. It orbits within a ~500 km wide "gap" or "notch" in the ring.[2][11] The gap is clearly somehow related to the moon but the origin of this connection has not been established. Metis supplies a significant part of the main ring's dust.[12] This material appears to consist primarily of material that is ejected from the surfaces of Jupiter's four small inner satellites by meteorite impacts. It is easy for the impact ejecta to be lost from the satellites into space because the satellites' surfaces lie fairly close to the edge of their Roche spheres due to their low density.[2]

See alsoEdit


  1. ^ a b c d Calculated on the basis of other parameters.


Cited sources

  • Anderson, J. D.; Johnson, T. V.; Schubert, G.; Asmar, S.; Jacobson, R. A.; Johnston, D.; Lau, E. L.; Lewis, G.; Moore, W. B.; Taylor, A.; Thomas, P. C.; Weinwurm, G. (27 May 2005). "Amalthea's Density is Less Than That of Water". Science. 308 (5726): 1291–1293. Bibcode:2005Sci...308.1291A. doi:10.1126/science.1110422. PMID 15919987.
  • Burns, Joseph A.; Showalter, Mark R.; Hamilton, Douglas P.; Nicholson, Philip D.; de Pater, Imke; Ockert-Bell, Maureen E.; Thomas, Peter C. (14 May 1999). "The Formation of Jupiter's Faint Rings". Science. 284 (5417): 1146–1150. Bibcode:1999Sci...284.1146B. doi:10.1126/science.284.5417.1146. PMID 10325220.
  • Burns, Joseph A.; Simonelli, Damon P.; Showalter, Mark R.; Hamilton, Douglas P.; Porco, Carolyn C.; Throop, Henry; Esposito, Larry W. (2004). "Jupiter's Ring-Moon System" (PDF). In Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (eds.). Jupiter: The Planet, Satellites and Magnetosphere. Cambridge University Press. pp. 241–262. ISBN 978-0-521-81808-7.
  • Evans, M. W.; Porco, C. C.; Hamilton, D. P. (September 2002). "The Orbits of Metis and Adrastea: The Origin and Significance of their Inclinations". Bulletin of the American Astronomical Society. 34: 883. Bibcode:2002DPS....34.2403E.
  • Marsden, Brian G. (August 26, 1980). "Satellites of Jupiter". IAU Circular. 3507. Retrieved 2012-03-28. (discovery)
  • Marsden, Brian G. (September 30, 1983). "Satellites of Jupiter and Saturn". IAU Circular. 3872. Retrieved 2012-03-28. (naming the moon)
  • Ockert-Bell, M. E.; Burns, J. A.; Daubar, I. J.; Thomas, P. C.; Veverka, J.; Belton, M. J. S.; Klaasen, K. P. (1 April 1999). "The Structure of Jupiter's Ring System as Revealed by the Galileo Imaging Experiment". Icarus. 138 (2): 188–213. Bibcode:1999Icar..138..188O. doi:10.1006/icar.1998.6072.
  • Simonelli, D. P.; Rossier, L.; Thomas, P. C.; Veverka, J.; Burns, J. A.; Belton, M. J. S. (October 2000). "Leading/Trailing Albedo Asymmetries of Thebe, Amalthea, and Metis". Icarus. 147 (2): 353–365. Bibcode:2000Icar..147..353S. doi:10.1006/icar.2000.6474.
  • Synnott, S. P. (19 June 1981). "1979J3: Discovery of a Previously Unknown Satellite of Jupiter". Science. 212 (4501): 1392. Bibcode:1981Sci...212.1392S. doi:10.1126/science.212.4501.1392. ISSN 0036-8075. PMID 17746259.
  • Thomas, P. C.; Burns, J. A.; Rossier, L.; Simonelli, D.; Veverka, J.; Chapman, C. R.; Klaasen, K.; Johnson, T. V.; Belton, M. J. S.; Galileo Solid State Imaging Team (September 1998). "The Small Inner Satellites of Jupiter". Icarus. 135 (1): 360–371. Bibcode:1998Icar..135..360T. doi:10.1006/icar.1998.5976.

External linksEdit