(158) Coronis
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Asteroid (158) coronis |
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| A three-dimensional model of (158) coronis based on its light curve | |
| Properties of the orbit ( animation ) | |
| Orbit type | Outer main belt |
| Asteroid family | Koronis family |
| Major semi-axis | 2.8685 AU |
| eccentricity | 0.0530 |
| Perihelion - aphelion | 2.7164 AU - 3.0206 AU |
| Inclination of the orbit plane | 1.0015 ° |
| Length of the ascending node | 278.0066 ° |
| Argument of the periapsis | 141.9823 ° |
| Time of passage of the perihelion | 4th July 2011 |
| Sidereal period | 4 a 316 d |
| Mean orbital velocity | 17.6 km / s |
| Physical Properties | |
| Medium diameter | 35.37 km (± 1.4) |
| Albedo | 0.2766 (± 0.024) |
| Rotation period | 14 h 13 min |
| Absolute brightness | 9.27 likes |
| Spectral class | S. |
| history | |
| Explorer | Viktor Knorre |
| Date of discovery | January 4, 1876 |
| Another name | 1955 HA 1 , A893 PA, A911 HB |
| Source: Unless otherwise stated, the data comes from JPL Small-Body Database Browser . The affiliation to an asteroid family is automatically determined from the AstDyS-2 database . Please also note the note on asteroid items. | |
(158) Koronis is an asteroid of the main belt , on 4 January 1876 by the Russian astronomer Viktor Knorre was discovered.
The origin of the name is unclear, the asteroid could be named after Koronis , a heroin from Greek mythology and mother of Asclepius (Aesculapia), or after Koronis , a nymph of the Hyades .
The coronis asteroid family is named after him.
According to its spectrum, it is classified as an S-asteroid . Photometric observations show a synodic rotation period of 14.206 ± 0.002 hours with a brightness fluctuation of 0.28-0.43. A subsequent study at the Altimira Observatory in 2010 agreed with this estimate and found a rotation period of 14.208 ± 0.040 hours. Based on a model constructed from the light curve, the shape of Koronis is similar to that of (243) Ida , an asteroid from the same family, although it is slightly larger.
A collision with (158) Koronis 15 million years ago created a group of 246 objects. (158) Koronis itself retained 98.7% of its total mass. The Koronis family (2) formed the new properties. Koronis (2) is a subfamily of the much larger Koronis family.
See also
Individual evidence
- ^ Dictionary of Minor Planet Names, Volume 1 in the Google Book Search
- ↑ DeMeo, Francesca E .; et al .: An extension of the Bus asteroid taxonomy into the near-infrared . In: Icarus . July 2009, p. 160–180 , bibcode : 2009Icar..202..160D ( archive.org [PDF] See Appendix A.).
- ↑ Slivan, Stephen M .; et al .: Spin vectors in the Koronis family: comprehensive results from two independent analyzes of 213 rotation lightcurves . In: Icarus . No. 162 (2) , April 2003, pp. 285–307 , doi : 10.1016 / S0019-1035 (03) 00029-0 , bibcode : 2003Icar..162..285S .
- ^ Buchheim, Robert K .: Phase Curves of 158 Koronis and 535 Montague . In: The Minor Planet Bulletin . No. 38 (3) , July 2011, p. 128–130 , bibcode : 2011MPBu ... 38..128B .
- ↑ Asteroid Models. (No longer available online.) Archived from the original on April 19, 2003 ; accessed on October 10, 2018 (English).
- ↑ Molnar, Lawrence A .; Haegert, MJ: Details of Recent Collisions of Asteroids 832 Karin and 158 Koronis . In: American Astronomical Society . DPS meeting # 41, No. 27.05 , September 2009, bibcode : 2009DPS .... 41.2705M .