(55638) 2002 VE95
| Discovery[1] | |
|---|---|
| Discovered by | NEAT |
| Discovery date | 14 November 2002 |
| Designations | |
| MPC designation | 2002 VE95 |
| Plutino[2] | |
| Orbital characteristics[3] | |
| Epoch 13 January 2016 (JD 2457400.5) | |
| Uncertainty parameter 2 | |
| Observation arc | 9246 days (25.31 yr) |
| Aphelion | 50.686 AU (7.5825 Tm) (Q) |
| Perihelion | 28.010 AU (4.1902 Tm) (q) |
| 39.348 AU (5.8864 Tm) (a) | |
| Eccentricity | 0.28814 (e) |
| 246.83 yr (90153.9 d) | |
| 20.605° (M) | |
| Inclination | 16.339° (i) |
| 199.90° (Ω) | |
| 207.41° (ω) | |
| Earth MOID | 27.0273 AU (4.04323 Tm) |
| Jupiter MOID | 23.0566 AU (3.44922 Tm) |
| Physical characteristics | |
| Dimensions | 249.8+13.5 −13.1[4] |
| 6.76 h (0.282 d) | |
|
Sidereal rotation period
|
6–9 h[5] |
| 0.149+0.019 −0.016[4] |
|
| B−V=1.07±0.14 V−R=0.72±0.05 B−R=1.79±0.04 R−I=0.76±0.12 V−I=1.38±0.15 B−I=2.47±0.13[4] |
|
| 20.5[6] | |
| 5.70±0.06,[4] 5.6[3] | |
(55638) 2002 VE95, also written as 2002 VE95, is a trans-Neptunian object (TNO) with an absolute magnitude of 5.7.[4] A 2:3 orbital resonance with Neptune makes it a plutino.[2]
Orbit and rotation
As a plutino 2002 VE95 is locked in 2:3 resonance with Neptune. This means that the ratio of their orbital periods is equal to 3/2.[2] It has been observed 190 times over 8 oppositions with precovery images back to 1990.[3]
The rotation period of 2002 VE95 is unknown but it probably lies between 6 and 9 hours.[5]
Physical characteristics
The size of 2002 VE95 is estimated at 249.8+13.5
−13.1 km, based on the Herschel Space Telescope measurements of the thermal radiation coming from it.[4] In the visible light this object is from moderately red to very red in color (different observations produced different results) and has a featureless reflectance spectrum.[7]
The near-infrared spectrum of 2002 VE95 is flat with two distinct absorption bands of water ice at 1.5 and 2.0 μm. There is the third feature near 2.3 μm of unclear origin.[8] The spectral behavior of this object is similar to 5145 Pholus, a centaur.[8] The surface of 2002 VE95 is heterogeneous—the amount of different ices and non-ice components depends on the observed area. Among the probable surface materials are water ice, methanol ice and various titan/triton tholins. The methanol ice is generally associated with redder areas. The surface of 2002 VE95 appears to be primordial in origin.[9]
References
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 2.0 2.1 2.2 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 4.2 4.3 4.4 4.5 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 5.0 5.1 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.
- ↑ 8.0 8.1 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
External links
- Orbital simulation from JPL (Java) / Horizons Ephemeris
- (55638) 2002 VE95 at the JPL Small-Body Database
