104 Klymene
| Discovery | |
|---|---|
| Discovered by | James Craig Watson |
| Discovery date | 13 September 1868 |
| Designations | |
| Main belt | |
| Orbital characteristics[1] | |
| Epoch 31 July 2016 (JD 2457600.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 130.58 yr (47693 d) |
| Aphelion | 3.6499 AU (546.02 Gm) |
| Perihelion | 2.65525 AU (397.220 Gm) |
| 3.15256 AU (471.616 Gm) | |
| Eccentricity | 0.15775 |
| 5.60 yr (2044.5 d) | |
Average orbital speed | 16.67 km/s |
| 101.498° | |
| 0° 10m 33.888s / day | |
| Inclination | 2.7905° |
| 41.698° | |
| 32.134° | |
| Earth MOID | 1.66901 AU (249.680 Gm) |
| Jupiter MOID | 1.63907 AU (245.201 Gm) |
| Jupiter Tisserand parameter | 3.186 |
| Physical characteristics | |
| Dimensions | 123.68±3.1 km |
| Mass | 2.0×1018 kg |
Equatorial surface gravity | 0.0346 m/s² |
Equatorial escape velocity | 0.0654 km/s |
| 8.984 h (0.3743 d) | |
| 0.0568±0.003 | |
| Temperature | ~157 K |
| C | |
| 8.27 | |
|
| |
104 Klymene is a large, dark Themistian asteroid that was discovered by J. C. Watson on September 13, 1868, and named after one of the many Clymenes in Greek mythology.[2] It is classified as a C-type asteroid, indicating it probably has a carbonaceous composition. The spectra indicates the presence of aqueous-altered minerals on the surface.[3]
Based upon measurements made using adaptive optics at the W. M. Keck Observatory, this object may have a bi-lobed shape with a length of 163 ± 3 km and width of 103 ± 5 km, for an average dimension of 133 km.[4] This asteroid is a member of the Themis family of asteroids that share similar orbital elements.[5] It is listed as a member of the Hecuba group of asteroids that orbit near the 2:1 mean-motion resonance with Jupiter.[6]
References
- ↑ Yeomans, Donald K., "104 Klymene", JPL Small-Body Database Browser, NASA Jet Propulsion Laboratory, retrieved 12 May 2016.
- ↑ Dictionary of minor planet names. p. 25. International Astronomical Union. 2003. Springer
- ↑ Fornasier, S.; et al. (February 1999), "Spectroscopic comparison of aqueous altered asteroids with CM2 carbonaceous chondrite meteorites", Astronomy and Astrophysics Supplement Series, 135 (1): 65–73, Bibcode:1999A&AS..135...65F, doi:10.1051/aas:1999161.
- ↑ Marchis, F.; et al. (November 2006), "Shape, size and multiplicity of main-belt asteroids. I. Keck Adaptive Optics survey", Icarus, 185 (1), pp. 39–63, Bibcode:2006Icar..185...39M, doi:10.1016/j.icarus.2006.06.001, PMC 2600456
, PMID 19081813. - ↑ Moore, Patrick; Rees, Robin, eds. (2011), "Patrick Moore's Data Book of Astronomy", Patrick Moore's Data Book of Astronomy by Patrick Moore and Robin Rees. Cambridge University Press (2nd ed.), Cambridge University Press: 165, Bibcode:2011pmdb.book.....M, ISBN 9781139495226.
- ↑ McDonald, Sophia Levy (June 1948), "General perturbations and mean elements, with representations of 35 minor planets of the Hecuba group", Astronomical Journal, 53, p. 199, Bibcode:1948AJ.....53..199M, doi:10.1086/106097.
