Metis/ˈmiːtəs/, 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.
Metis is tidally lockedtoJupiter, and its shape is strongly asymmetrical, with the largest diameter 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 ring material.
Voyager 1 discovery image of Metis on 4 March 1979, showing the moon's tiny silhouette against the backdrop of Jupiter's clouds
Metis was discovered in 1979 by Stephen P. Synnott in images taken by the Voyager 1 probe and was provisionally designatedasS/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 equivalentofJupiter).[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.[4]
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]
Metis has an irregular shape and measures 60 km × 40 km × 34 km across, which makes it the second smallest of the four inner satellites of Jupiter.[4] Therefore, a very rough estimate of its surface area could be placed between 5,800 and 11,600 square kilometers (approx. 8,700).[citation needed] The bulk composition and mass of Metis are not known, but it is likely that its mean density is 1.5 g/cm3 or higher,[10] and its mass can therefore be estimated as ~6.4×1016 kg or higher.
The surface of Metis is heavily cratered, dark, and appears to be reddish in color. There is a substantial asymmetry between the 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 excavates a bright material (presumably ice) from its interior.[5]
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.[2][3]
Due to tidal locking, Metis rotates synchronously with its orbital period (about 7 hours), with its longest axis aligned towards Jupiter.[3][4] Jupiter casts a shadow on all of Metis for 68 minutes each Metian day.[a]
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.[3]
Metis orbiting at the edge of Jupiter's Main Ring, as imaged by the New Horizons spacecraft on 24 February 2007
Metis's orbit lies ~1,000 km within the main ring of Jupiter. It orbits within a ~500 km wide "gap" or "notch" in the ring.[3][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.[3]
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. PMID15919987. S2CID924257.
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. Bibcode:2004jpsm.book..241B. ISBN978-0-521-81808-7.
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)
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