(434620) 2005 VD
| Designations | |
|---|---|
| MPC designation | 2005 VD |
| damocloid[3] | |
| Orbital characteristics[1] | |
| Epoch December 9, 2014 (2457000.5) | |
| Aphelion | 8.33816 AU (Q) |
| Perihelion |
4.986316 AU (q) (near Jupiter) |
| 6.66224 AU (a) | |
| Eccentricity | 0.251555 |
| 17.20 yr (6281.00 days) | |
| 181.9842° (M) | |
| Inclination | 172.8655 ° |
| 173.2640° | |
| 178.8839° | |
| Jupiter MOID | 0.0187 AU |
| Physical characteristics | |
| Dimensions | ~9.6 km |
| 0.04 (assumed dark) | |
| 14.2[1] | |
|
| |
(434620) 2005 VD is a centaur and damocloid. It has the second most highly inclined orbit of any known object in the solar system, second to 2013 LA2. It was the most highly inclined known object between 2005 and 2013.
Classification
2005 VD has a semi-major axis greater than Jupiter and almost crosses the orbit of Jupiter when near perihelion. JPL lists it as a current centaur.[1] Both the Deep Ecliptic Survey (DES),[2] and the Minor Planet Center (MPC)[4] have listed it as a centaur (qmin=~5AU) at different epochs. The DES and MPC will list as a centaur again in 2032.
Lowell Observatory also has it listed as a damocloid object.[3]
2005 VD makes occasional close approaches to Jupiter, coming only 0.0817 AU from Jupiter in 1903, 0.0444 AU in 2057, and 0.077 AU in 2093. However the closest approach it will make in the next decade will only be 0.3089 AU on December 17, 2022.[1]
References
- 1 2 3 4 5 "JPL Small-Body Database Browser: (2005 VD)" (last observation: 2013-05-14). Retrieved 2008-10-10.
- 1 2 Marc W. Buie (2006-08-28). "Orbit Fit and Astrometric record for 05VD". SwRI (Space Science Department). Retrieved 2008-10-10. (Webcite from 2009-09-02)
- 1 2 Akimasa Nakamura (2009-05-02). "Table of Damocloid objects, or Oort cloud asteroids". Lowell Observatory. Retrieved 2014-11-14.
- ↑ "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 2010-07-16. (WayBackMachine from 12 April 2013)
External links
- Orbital simulation from JPL (Java) / Ephemeris