2005 VX3
Trans-Neptunian object
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2005 VX3 is a trans-Neptunian object and retrograde damocloid on a highly eccentric, cometary-like orbit. It was first observed on 1 November 2005, by astronomers with the Mount Lemmon Survey at the Mount Lemmon Observatory in Arizona, United States. The unusual object measures approximately 7 kilometers (4 miles) in diameter.[4] It has the 3rd largest known heliocentric semi-major axis and aphelion.[6] Additionally its perihelion lies within the orbit of Jupiter, which means it also has the largest orbital eccentricity of any known minor planet.
| Discovery[1][2] | |
|---|---|
| Discovered by | Mount Lemmon Srvy. |
| Discovery site | Mount Lemmon Obs. (first observed only) |
| Discovery date | 1 November 2005 |
| Designations | |
| 2005 VX3 | |
| TNO[3] · damocloid[4] unusual[5] · distant[1] | |
| Orbital characteristics[3] | |
| Epoch 21 November 2025 (JD 2461000.5) | |
| Uncertainty parameter 4 | |
| Observation arc | 81 days |
| Aphelion | 2124.24 AU |
| Perihelion | 4.1435 AU |
| 1064.19 AU | |
| Eccentricity | 0.9961 |
| 34,717 yr | |
| 0.2061° | |
| 0° 0m 0.101s / day | |
| Inclination | 112.69° |
| 255.11° | |
| 196.48° | |
| Jupiter MOID | 0.8405 AU |
| TJupiter | −0.968 |
| Physical characteristics | |
| 7 km (est.)[4] | |
| 0.09 (assumed)[4] | |
| 14.1[1][3] | |
Description
2005 VX3 orbits the Sun at a distance of 4.1–2,124 AU once every 34,717 years (semi-major axis of 1,064 AU). Its orbit has an eccentricity of 0.9961 and an inclination of 113° with respect to the ecliptic. It belongs to the dynamical group of damocloids due to its retrograde orbit and its low Tisserand parameter (TJupiter of −0.968).[3] It is a Jupiter-, Saturn-, Uranus-, and Neptune-crosser. The body's observation arc begins with its first observation by the Mount Lemmon Survey on 1 November 2005.[1]
2005 VX3 has a barycentric semi-major axis of ~1026 AU.[7][a] 2014 FE72 and (668643) 2012 DR30 have a larger barycentric semi-major axis. The epoch of January 2016 was when 2005 VX3 had its largest heliocentric semi-major axis.
The object has a short observation arc of 81 days and does not have a well constrained orbit.[3] It has not been observed since January 2006, when it came to perihelion, 4.1 AU from the Sun.[3] It may be a dormant comet that has not been seen outgassing. In the past it may have made closer approaches to the Sun that could have removed most near-surface volatiles. The current orbit crosses the ecliptic just inside Jupiter's orbit and has a Jupiter-MOID of 0.8 AU.[3]
In 2017, it had an apparent magnitude of ~28 and was 24 AU from the Sun. It comes to opposition in mid-June.[year needed] It would require one of the largest telescopes in the world for any more follow-up observations.
Comparison
See also
Notes
- Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the semi-major axis and orbital period. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates.[8] Using JPL Horizons, the barycentric semi-major axis is approximately 1026 AU.[7]
- Archived JPL Small-Body Database Browser: (2005 VX3) from 13 December 2012. JPL Epoch 2012 orbital solution that has aphelion (Q)=1914 AU.
- Archived MPC object data for (2005 VX3) from Minor Planet Center archive of Epoch 2015-06-27 with aphelion (Q) of 2563 AU.
- Archived MPC object data for (2005 VX3) from JPL Webcite archive of Epoch 2016-Jan-13 with aphelion (Q) of 3235AU.
- [e]Archived MPC object data for (2005 VX3) from 8 March 2014.