22 Kalliope
| Discovery | |
|---|---|
| Discovered by | John Russell Hind |
| Discovery date | November 16, 1852 |
| Designations | |
| none | |
| Main belt | |
| Orbital characteristics | |
| Epoch November 12, 2005 (JD 2453686.5) | |
| Aphelion | 479.931 Gm (3.208 AU) |
| Perihelion | 390.433 Gm (2.610 AU) |
| 435.182 Gm (2.909 AU) | |
| Eccentricity | 0.103 |
| 1812.245 d (4.96 a) | |
Average orbital speed | 17.42 km/s |
| 303.545° | |
| Inclination | 13.710° |
| 66.240° | |
| 356.172° | |
| Physical characteristics | |
| Dimensions | 215×180×150 km [1][2] |
| Mass | 6.3 ± 0.5 ×1018 kg [3][4] |
Mean density | 2.03 ± 0.16 g/cm³ [3] |
| 0.038 m/s² | |
| 0.09 km/s | |
| 0.1728 d (4.148 h) [5] | |
| Albedo | 0.142 [1] |
| Temperature | ~161 K max: 240 K (-32°C) |
Spectral type | M [6] |
| 6.45 | |
22 Kalliope is a big main belt asteroid of the M-type, found by J. R. Hind on November 16, 1852. It is named after Calliope, the Greek Muse of epic poetry.
Characteristics
Kalliope is about 180 km in diameter but is not perfectly round, as shown by images from the VLT at the European Southern Observatory [7]
Its spectrum is M-type, but Kalliope does not appear to be metallic. It is similar to other M-types such as 21 Lutetia. Firstly, its density is far too low to be metal. Second, spectroscopic studies have shown evidence of hydrated minerals [8] and silicates,[9] so the surface is probably stony. Kalliope also has a low radar albedo,[4] unlike most metallic surfaces.
Lightcurve analysis indicates that Kalliope's pole most likely points towards ecliptic coordinates (β, λ) = (-23°, 20°) with a 10° uncertainty,[2][3] which gives Kalliope an axial tilt of 103°. Kalliope's rotation is then a bit retrograde.
Moon
Kalliope has one known moon, Linus, or (22) Kalliope I Linus. It is quite big: 30–40 km in diameter. It orbits about 1065 km from Kalliope. This is about 12 times the radius of Kalliope. Linus was found on August 29, 2001 by Jean-Luc Margot and Michael E. Brown, while another team also independently found the moon 3 days later.[7]
References
- ↑ 1.0 1.1 "Supplemental IRAS Minor Planet Survey". Archived from the original on 2006-06-23. Retrieved 2007-12-19.
- ↑ 2.0 2.1 M. Kaasalainen; et al. (2002). "Models of Twenty Asteroids from Photometric Data" (PDF). Icarus. 159 (2): 369. doi:10.1006/icar.2002.6907. Archived from the original (PDF) on 2008-02-16. Retrieved 2007-12-19.
- ↑ 3.0 3.1 3.2 F. Marchis; et al. (2003). "A three-dimensional solution for the orbit of the asteroidal satellite of 22 Kalliope". Icarus. 165 (1): 112. Bibcode:2003Icar..165..112M. doi:10.1016/S0019-1035(03)00195-7.
- ↑ 4.0 4.1 J.L. Margot & M.E. Brown (2003). "A Low-Density M-type Asteroid in the Main Belt". Science. 300 (5627): 1939–1942. Bibcode:2003Sci...300.1939M. doi:10.1126/science.1085844. PMID 12817147. S2CID 5479442.
- ↑ "PDS lightcurve data". Archived from the original on 2006-06-14. Retrieved 2007-12-19.
- ↑ "PDS spectral class data". Archived from the original on 2010-01-17. Retrieved 2007-12-19.
{cite web}: CS1 maint: bot: original URL status unknown (link) - ↑ 7.0 7.1 synthesis of several observations including recent ones with the VLT 8m telescope.
- ↑ A.S. Rivkin; et al. (2000). "The nature of M-class asteroids from 3-micron observations". Icarus. 145 (2): 351. Bibcode:2000Icar..145..351R. doi:10.1006/icar.2000.6354.
- ↑ D.F. Lupishko; et al. (1982). "UBV photometry of the M-type asteroids 16 Psyche and 22 Kalliope". Solar System Research. 16: 75.
Other websites
- Kalliope and Linus very well resolved with the 8m VLT at ESO. Also includes a Kalliope shape model.
- shape model deduced from lightcurve Archived 2008-02-16 at the Wayback Machine
- orbit diagram for Linus Archived 2006-06-15 at the Wayback Machine
- A different VLT image of Kalliope and Linus Archived 2006-09-28 at the Wayback Machine
- Data sheet at Johnston's Archive, includes some other parameters.