Image of Adrastea taken by Galileo's solid state imaging system between November 1996 and June 1997.
|Discovered by||David C. Jewitt
G. Edward Danielson
|Discovery time||July 8, 1979|
|Avg. distance from the center of its orbital path||129,000 km|
|How egg-shaped its orbit is
|How long it takes to complete an orbit||0.29826 d (7 h 9.5 min)|
|Average speed||31.378 km/s|
|Angle above the reference plane
|0.03° (to Jupiter's equator)|
|What it orbits||Jupiter|
|Size and Other Qualities|
|Average distance from its center to its surface||8.2 ± 2.0 km|
|Volume inside it||~2,345 km³|
|Average density||0.86 g/cm³ (assumed)|
|Gravity at its surface||~0.002 m/s² (0.0004 g)|
|Slowest speed able to escape into space
|How long it takes to turn around one time||synchronous|
|Angle at which it turns
(in relation to its orbit)
|How much light it reflects||~0.1 ± 0.045|
|Avg. surface temp.||~122 K|
Adrastea or Jupiter XV, is the second closest moon to Jupiter. It was found by David C. Jewitt and G. Edward Danielson in Voyager 2 probe photographs taken in 1979 and received the designation S/1979 J 1. In 1983, it was named after the mythological Adrastea, who was a daughter of Jupiter and Ananke.
Adrastea was the first moon to be found from images taken by an interplanetary spacecraft, rather than through telescopic photography.
Physical characteristics[change | change source]
Adrastea is non-spherical and measures 20x16x14 km³ across. What Adrastea is made of and the mass of Adrastea are not known, but assuming that its mean density is like that of Amalthea (~0.86 g/cm³) its mass can be estimated at ~2×1015 kg. Amalthea's density implies that moon is composed of water ice with a porosity of 10-15%, and Adrastea may be similar.
No surface details of Adrastea are known, due to the low resolution of available images.
Orbit[change | change source]
Adrastea is the smallest and second closest member of the closer moons to Jupiter. It orbits Jupiter at ~129,000 km (1.806 Jupiter radii) within the planet's Main Ring. The orbital eccentricity of ~0.0015 and inclination of ~ 0.03° relative to the equator of Jupiter are very small.
Exploration[change | change source]
References[change | change source]
- Evans, M.W.; Porco, C.C.; Hamilton, D.P. (2002). "The Orbits of Metis and Adrastea: The Origin and Significance of their Inclinations". Bulletin of the American Astronomical Society 34: 883. http://adsabs.harvard.edu/abs/2002DPS....34.2403E.
- Burns, J.A.; D.P. Simonelli & M.R. Showalter et al. (2004), "Jupiter’s Ring-Moon System", in Bagenal, F.; Dowling, T. E.; McKinnon, W. B., Jupiter: The planet, Satellites and Magnetosphere, Cambridge University Press
- Calculated on the basis of other parameters
- Thomas, P.C.; Burns, J.A.; Rossier, L.; et al. (1998). "The Small Inner Satellites of Jupiter". ICARUS 135: 360–371. doi:10.1006/icar.1998.5976. http://adsabs.harvard.edu/abs/2000Icar..147..353S.
- IAUC 3454: Editorial Notice 1980 February 25 (discovery)
- Jewitt, D.C.; Danielson, G.E.; Synnott, S.P. (1979). "Discovery of a New Jupiter Satellite". Science 206: 951. http://links.jstor.org/sici?sici=0036-8075%2819791123%293206:4421%3c951:DOANJS%3e2.0.CO%3b2-V&origin=ads.
- IAUC 3872: Satellites of Jupiter and Saturn 1983 September 30 (naming the moon)
- Anderson, J.D.; Johnson, T.V.; Shubert, G.; et al. (2005). "Amalthea’s Density Is Less Than That of Water". Science 308: 1291–1293. doi:10.1126/science.1110422. http://adsabs.harvard.edu/abs/2005Sci...308.1291A.
Other websites[change | change source]