Image of Thebe taken by the Galileo spacecraft on 4 January 2000
|Discovered by||Stephen P. Synnott / Voyager 1|
|Discovery date||5 March 1979|
Mean orbit radius
|889.0±0.6 km ( 2213.11 RJ)|
|536±0.000001 d (16 h 11.3 min) 0.674|
Average orbital speed
|23.92 km/s (calculated)|
|Inclination||±0.003° (to Jupiter's equator) 1.076°|
|Dimensions||116 × 98 × 84 km|
|Volume||000 km3≈ 500|
|(0.004 g) 0.013 m/s<sup<2>[c]|
|Temperature||≈ 124 K|
Thebe (// THEE-bee; Greek: Θήβη) also known as Jupiter XIV, is the fourth of Jupiter's moons by distance from the planet. It was discovered by Stephen P. Synnott in images from the Voyager 1 space probe taken on March 5, 1979, while making its flyby of Jupiter. In 1983 it was officially named after the mythological nymph Thebe.
The second largest of the inner satellites of Jupiter, Thebe orbits within the outer edge of the Thebe gossamer ring that is formed from dust ejected from its surface. It is irregularly shaped and reddish in colour, and is thought like Amalthea to consist of porous water ice with unknown amounts of other materials. Its surface features include large craters and high mountains—some of them are comparable to the size of the moon itself.
Discovery and observations
Thebe was discovered by Stephen P. Synnott in images from the Voyager 1 space probe taken on March 5, 1979, and was initially given the provisional designation S/1979 J 2. In 1983 it was officially named after the mythological nymph Thebe who was a lover of Zeus—the Greek equivalent of Jupiter.
After its discovery by Voyager 1, Thebe was photographed by the Voyager 2 space probe in 1979. However, before the Galileo spacecraft arrived at Jupiter, knowledge about it was extremely limited. Galileo imaged almost all of the surface of Thebe and helped clarify its composition.
Thebe is the outermost of the inner Jovian moons, and orbits Jupiter at a distance of about 222,000 km (3.11 Jupiter radii). Its orbit has an eccentricity of 0.018, and an inclination of 1.08° relative to the equator of Jupiter. These values are unusually high for an inner satellite and can be explained by the past influence of the innermost Galilean satellite, Io; in the past, several mean-motion resonances with Io would have passed through Thebe's orbit as Io gradually receded from Jupiter, and these excited Thebe's orbit.
The orbit of Thebe lies near the outer edge of the Thebe gossamer ring, which is composed of the dust ejected from the satellite. After ejection the dust drifts in the direction of the planet under the action of Poynting–Robertson drag forming a ring inward of the moon.
Thebe is irregularly shaped, with the closest ellipsoidal approximation being 116×98×84 km. Its surface area is probably between 31,000 and 59,000 (~45,000) km2. Its bulk density and mass are not known, but assuming that its mean density is like that of Amalthea (around 0.86 g/cm3), its mass can be estimated at roughly 4.3 × 1017 kg.
Similarly to all inner satellites of Jupiter, Thebe rotates synchronously with its orbital motion, thus keeping one face always looking toward the planet. Its orientation is such that the long axis always points to Jupiter. At the surface points closest to and furthest from Jupiter, the surface is thought to be near the edge of the Roche lobe, where Thebe's gravity is only slightly larger than the centrifugal force. As a result, the escape velocity in these two points is very small, thus allowing dust to escape easily after meteorite impacts, and ejecting it into the Thebe gossamer ring.
Zethus Crater is the largest (diameter about 40 km) crater on and the only named surface feature of Jupiter's moon Thebe. There are several bright spots at the rim of this crater. It is located on the far side of Thebe, facing away from Jupiter. It was discovered by the Galileo spacecraft. It is named for Zethus, the husband of the nymph Thebe in Greek mythology.
The surface of Thebe is 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 (probably ice) from the interior of the moon. The surface of Thebe is heavily cratered and it appears that there are at least three or four impact craters that are very large, each being roughly comparable in size to Thebe itself.
- Calculated as a×(1 − e), where a is semimajor axis and e is eccentricity.
- Calculated as a×(1 + e), where a is semimajor axis and e is eccentricity.
- The estimate from Thomas, 1998 was divided by 1.5 to account for the difference in assumed densities.
- The estimate from Burns, 2004 was divided by 1.5 to account for the difference in assumed densities.
- Cooper Murray et al. 2006.
- Thomas Burns et al. 1998.
- Burns Simonelli et al. 2004.
- Simonelli Rossier et al. 2000.
- Synnott 1980.
- IAUC 3872.
- IAUC 3470.
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- 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.
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- USGS/IAU. "Zethus on Thebe". Gazetteer of Planetary Nomenclature. USGS Astrogeology. Retrieved 2012-03-27.