(84922) 2003 VS2
|
|
| Discovery[2] | |
|---|---|
| Discovered by | NEAT (644) |
| Discovery date | November 14, 2003[1] |
| Designations | |
| MPC designation | (84922) 2003 VS2 |
| none | |
| Plutino[3][4] | |
| Orbital characteristics[1][3] | |
| Epoch December 31, 2006 (JD 2454100.5) | |
| Aphelion | 42.104 AU (6298.735 Gm) |
| Perihelion | 36.427 AU (5449.350 Gm) |
| 39.266 AU (5874.042 Gm) | |
| Eccentricity | 0.072 |
| 246.05 a (89,870.237 d) | |
|
Average orbital speed
|
4.75 km/s |
| 3.987° | |
| Inclination | 14.798° |
| 302.682° | |
| 112.586° | |
| Physical characteristics | |
| Dimensions | 523.0+35.1 −34.4 km[5] |
|
Sidereal rotation period
|
7.41±0.02 h[6] |
| Albedo | 0.147+0.063 −0.043[5] |
| Temperature | ≈44 K |
|
Spectral type
|
(moderately red) B−V= 0.93±0.02 V−R= 0.59±0.02[5] |
| 19.7[7] | |
| 4.10±0.38[5] 4.4[8] 4.73±0.02[9] |
|
(84922) 2003 VS2 is a trans-Neptunian object discovered by the Near Earth Asteroid Tracking program on November 14, 2003.[2] Like Pluto, it is in a 2:3 orbital resonance with Neptune,[3][4] giving it the orbital properties of a plutino. Mike Brown's website lists it as highly likely a dwarf planet.[10] However, Brown assumed that VS2 was much bigger than it really is, and the light-curve analysis has questioned whether it would truly be in the hydrostatic equilibrium.[11]
Orbit and rotation
Like Pluto, (84922) 2003 VS2 is locked in the 3:2 mean-motion resonance with Neptune, although its orbit is significantly less eccentric than Pluto's. It also has slightly smaller orbital inclination.[1]
(84922) 2003 VS2 has a significant light-curve amplitude of 0.21±0.01. The most likely value of the rotation period is 7.41±0.02 h.[6]
Physical characteristics
(84922) 2003 VS2 has a moderately red surface with a moderately red color indexes B−V=0.93, V−R=0.59.[9] Its geometrical albedo is about 15%.[5]
In 2007, its diameter was initially estimated by the Spitzer Space Telescope at 725±200 km.[8] However, in 2012, this was reduced to 523.0+35.1
−34.4 km after new Herschel Space Telescope observations.[5] The latter measurement is considered more reliable. Assuming a Pluto-like density of 2 g/cm3, one can obtain a mass estimate of about 1.5×1020 kg.
References
- ↑ 1.0 1.1 1.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 2.0 2.1 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 3.0 3.1 3.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 4.0 4.1 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 6.0 6.1 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 8.0 8.1 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 9.0 9.1 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found. (Dwarf Planet & Plutoid Headquarters)
External links
- Orbital simulation from JPL (Java) / Ephemeris
- Huge rock-ice body circles Sun (Palomar Photo)
- 2003 VS2 precovery (18 Nov. '03 Major News about Minor Objects)
