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Adrastea (moon)

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For the moon of Jupiter known by this name between 1955 and 1975, see Ananke (moon).

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Adrastea
Image of Adrastea taken by Galileo spacecraft between November 1996 and June 1997
Discovery
Discovered by
Discovery date8 July 1979
Designations
AdjectivesAdrastean
Orbital characteristics
Mean orbit radius
129000 km[1][2]
Eccentricity0.0015[1][2]
0.29826 d
(7 h, 9.5 min)[1][2]
31.378 km/s[a]
Inclination0.03°
(to Jupiter's equator)[1][2]
Satellite ofJupiter
Physical characteristics
Dimensions20 × 16 × 14 km[3]
8.2±2.0 km[3]
Volume≈ 2345 km3[a]
synchronous
zero[3]
Albedo0.10±0.045[3]
Temperature≈ 122 K

Adrastea (/ædrəˈstiːə/ ad-rə-STEE-ə; Template:Lang-el), also known as Jupiter XV, is the second by distance, and the smallest of the four inner moons of Jupiter. It was discovered in photographs taken by Voyager 2 in 1979, making it the first natural satellite to be discovered from images taken by an interplanetary spacecraft, rather than through a telescope.[4] It was officially named after the mythological Adrasteia, foster mother of the Greek god Zeus—the equivalent of the Roman god Jupiter.[5]

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 other than 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 fainter 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.[4][6] Although it appeared only as a dot,[6] 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 months earlier by Voyager 1. The Galileo spacecraft was able to determine the moon's shape in 1998, but the images remain poor.[3] In 1983, Adrastea was officially named after the Greek nymph Adrastea, the daughter of Zeus and his lover Ananke.[5]

Physical characteristics

Adrastea has an irregular shape and measures 20×16×14 km across.[3] A surface area estimate would be between 840 and 1,600 (~1,200) km2. This makes it 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,[7] its mass can be estimated at about 2 × 1015 kg. Amalthea's density implies that the moon is composed of water ice with a porosity of 10–15%, and Adrastea may be similar.[7]

No surface details of Adrastea are known, due to the low resolution of available images.[3]

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 one of only 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.[3]

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]

Adrastea is the second-fastest-moving of Jupiter's moons, with an orbital speed of 31.378 km/s.

Relationship with Jupiter's rings

Adrastea is the largest contributor to material in Jupiter's rings. This 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 due to the satellites' low density and their surfaces lying 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.[8] More precisely, the orbit of Adrastea lies near the outer edge of Jupiter's Main Ring.[9] 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,[9] 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 Calculated on the basis of other parameters.
  1. ^ a b c d Evans Porco et al. 2002.
  2. ^ a b c d e f g h i j Burns Simonelli et al. 2004.
  3. ^ a b c d e f g h Thomas Burns et al. 1998.
  4. ^ a b IAUC 3454.
  5. ^ a b IAUC 3872.
  6. ^ a b Jewitt Danielson et al. 1979.
  7. ^ a b Anderson Johnson et al. 2005.
  8. ^ Burns Showalter et al. 1999.
  9. ^ a b Ockert-Bell Burns et al. 1999.

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. Bibcode:2004jpsm.book..241B. 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.
  • Jewitt, David C.; Danielson, G. Edward; Synnott, Stephen P. (November 23, 1979). "Discovery of a New Jupiter Satellite". Science. 206 (4421): 951. Bibcode:1979Sci...206..951J. doi:10.1126/science.206.4421.951. PMID 17733911.
  • Marsden, Brian G. (February 25, 1980). "Editorial Notice". IAU Circular. 3454. Archived from the original on 2011-07-25. Retrieved 2012-03-28. {{cite journal}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help) (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.
  • 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.
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