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Adrastea (moon)

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For the asteroid, see 239 Adrastea.
For the moon of Jupiter known by this name between 1955 and 1975, see Ananke (moon).
Adrastea the great
Image of Adrastea taken by Galileo spacecraft between November 1996 and June 1997
Discovery
Discovered byDavid C. Jewitt
G. Edward Danielson
Discovery dateJuly 8, 1979
Orbital characteristics
Mean orbit radius
129,000 km[1][2]
Eccentricity0.0015[1][2]
0.29826 d
(7 h 9.5 min)[1][2]
31.378 km/s[3]
Inclination0.03°
(to Jupiter's equator)[1][2]
Satellite ofJupiter
Physical characteristics
Dimensions20×16×14 km[4]
8.2 ± 2.0 km[4]
Volume~2,345 km³[3]
Mass~2 kg[3]
Mean density
0.86 g/cm³ (assumed)
~0.002 m/s²
(0.0004 g)[3]
~0.008 km/s[3]
synchronous
zero[4]
Albedo0.1 ± 0.045[4]
Temperature~122 K

Adrastea (Template:Pron-en AD-rə-STEE-ə, or as in Greek Αδράστεια), also known as Jupiter XV, is the second by distance, and the smallest of the four inner moons of Jupiter. It was discovered in Voyager 2 probe photographs taken in 1979, making it the first natural satellite to be discovered from images taken by an interplanetary spacecraft, rather than through telescopic photography.[5] It was officially named after the mythological Adrastea, daughter of Greek god Zeus—the equivalent of Roman god Jupiter.[6] Adrastea is one of the few moons in the Solar System known to orbit its planet in less than the length of that planet's day. It orbits at the edge of Jupiter's Main Ring and is thought to be the main contributor of material to the Rings of Jupiter. Despite observations made in the 1990s by the Galileo spacecraft, very little is known about the moon's physical characteristics outside its size and the fact that it is tidally locked to Jupiter.

Discovery and observations

Discovery image of Adrastea, taken on July 8, 1979 by Voyager 2. Adrastea is the dot in the very middle, straddling the line of the Jovian rings.

Adrastea was discovered by David C. Jewitt and G. Edward Danielson in Voyager 2 probe photographs taken on July 8, 1979, and received the designation S/1979 J 1.[5][7] Although it appeared only as a dot,[7] it was the first moon to be discovered by an interplanetary spacecraft. Soon after its discovery, two other of the inner moons of Jupiter (Thebe and Metis) were observed in the images taken a few weeks earlier by Voyager 1. The Galileo spacecraft was able to determine the moon's shape in 1998, but the images remain poor.[4] In 1983, Adrastea was officially named after the Greek nymph Adrastea, the daughter of Zeus and his lover Ananke.[6]

Physical characteristics

Adrastea has an irregular shape and measures 20×16×14 km across.[4] This makes Adrastea the smallest of the four inner moons. The bulk, composition and mass of Adrastea are not known, but assuming that its mean density is like that of Amalthea,[2](around 0.86 g/cm³[8]) its mass can be estimated at about 2 kg. Amalthea's density implies that the moon is composed of water ice with a porosity of 10–15%, and Adrastea may be similar.[8]

No surface details of Adrastea are known, due to the low resolution of available images.[4]

Orbit

Adrastea is the smallest and second closest member of the inner Jovian satellite family. It orbits Jupiter at a radius of about 129,000 km (1.806 Jupiter radii) at the exterior edge of the planet's Main Ring.[2] Adrastea is only one of the three moons in the Solar System known to orbit its planet in less than the length of that planet's day—the other two being Jupiter's innermost moon Metis, and Mars' moon Phobos. The orbit has very small eccentricity and inclination—around 0.0015 and 0.03°, respectively. Inclination is relative to the equator of Jupiter.[2]

Due to tidal locking, Adrastea rotates synchronously with its orbital period, keeping one face always looking toward the planet. Its long axis is aligned towards Jupiter, this being the lowest energy configuration.[4]

The orbit of Adrastea lies inside Jupiter's synchronous orbit radius (as does Metis’s), and as a result, tidal forces are slowly causing its orbit to decay so that it will one day impact Jupiter. If its density is similar to Amalthea's then its orbit would actually lie within the fluid Roche limit. However, since it is not breaking up, it must still lie outside its rigid Roche limit.[2]

Relationship with Jupiter's rings

Adrastea is the largest contributor to material in Jupiter's rings. 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 these satellites into space. This is because, due to the satellites' low density, their surfaces lie rather close to the edge of their Roche spheres.[2]

It seems that Adrastea is the most copious source of this ring material, as evidenced by the densest ring (the Main Ring) being located at and within Adrastea's orbit.[9] More precisely, the orbit of Adrastea lies near the outer edge of Jupiter's Main Ring.[10] The exact extent of visible ring material depends on the phase angle of the images: in forward-scattered light Adrastea is firmly outside the Main Ring,[10] but in back-scattered light (which reveals much bigger particles) there appears to also be a narrow ringlet outside Adrastea's orbit.[2]

References

  1. ^ a b c d Evans, M.W. (2002). "The Orbits of Metis and Adrastea: The Origin and Significance of their Inclinations". Bulletin of the American Astronomical Society. 34: 883. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  2. ^ a b c d e f g h i j Burns, J.A. (2004). "Jupiter's Ring-Moon System" (pdf). In Bagenal, F.; Dowling, T.E.; McKinnon, W.B. (ed.). Jupiter: The Planet, Satellites and Magnetosphere. Cambridge University Press. {{cite encyclopedia}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)CS1 maint: multiple names: editors list (link)
  3. ^ a b c d e Calculated on the basis of other parameters.
  4. ^ a b c d e f g h Thomas, P.C. (1998). "The Small Inner Satellites of Jupiter". Icarus. 135: 360–371. doi:10.1006/icar.1998.5976. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  5. ^ a b Marsden, Brian G. (1980-02-25). "Editorial Notice". IAU Circulars. 3454. (discovery)
  6. ^ a b Marsden, Brian G. (1983-09-30). "Satellites of Jupiter and Saturn". IAU Circulars. 3872. (naming the moon)
  7. ^ a b Jewitt, D.C. (1979). "Discovery of a New Jupiter Satellite". Science. 206 (4421): 951. doi:10.1126/science.206.4421.951. PMID 17733911. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  8. ^ a b Anderson, J.D. (2005). "Amalthea's Density Is Less Than That of Water". Science. 308: 1291–1293. doi:10.1126/science.1110422. PMID 15919987. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  9. ^ Burns, J.A. (1999). "The Formation of Jupiter's Faint Rings". Science. 284: 1146–1150. doi:10.1126/science.284.5417.1146. PMID 10325220. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  10. ^ a b Ockert-Bell, M. E. (1999). "The Structure of Jupiter's Ring System as Revealed by the Galileo Imaging Experiment". Icarus. 138: 188–213. doi:10.1006/icar.1998.6072. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
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