(690420) 2014 FC72
| Discovery[1] | |
|---|---|
| Discovered by | Pan-STARRS 1 |
| Discovery site | Haleakala Obs. |
| Discovery date | 24 March 2014 (first observed only) |
| Designations | |
| 2014 FC72 | |
| Orbital characteristics[2] | |
| Epoch 27 April 2019 (JD 2458600.5) | |
| Uncertainty parameter 3 | |
| Observation arc | 16.91 yr (6,178 d) |
| Aphelion | 100.57 AU |
| Perihelion | 51.663 AU |
| 76.114 AU | |
| Eccentricity | 0.3212 |
| 664.06 yr (242,547 d) | |
| 357.23° | |
| 0° 0m 5.4s / day | |
| Inclination | 29.859° |
| 178.00° | |
| ≈ 25 November 2023[6] ±7 days | |
| 33.138° | |
| Physical characteristics | |
| 22.09[8] | |
| 4.7[1][2] | |
(690420) 2014 FC72 is a trans-Neptunian object, classified as a scattered and detached object, located in the outermost region of the Solar System. It was first observed on 24 March 2014 by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States.[1] With its perihelion distant from Neptune, it belongs to a small and poorly understood group of objects with moderate eccentricities.[9][10] It is estimated to measure 500 kilometers (300 miles) in diameter, assuming a low albedo.
Orbit and classification
[edit]
2014 FC72 orbits the Sun at a distance of 51.7–100.6 AU once every 664 years (242,547 days; semi-major axis of 76.11 AU). Its orbit has a moderate eccentricity of 0.32 and an inclination of 30° with respect to the ecliptic.[2]
The object belongs to the same orbital group as 2004 XR190 ("Buffy"), 2014 FZ71, 2015 FJ345 and 2015 KQ174 (also see diagram). With an orbital period of 664 years, they seem to be resonant trans-Neptunian objects in a 1:4 resonance with Neptune, as are 2003 LA7 and 2011 UP411,[5] but with lower eccentricities and therefore higher perihelia as the latter.
Considered a scattered and detached object,[3][4][5] 2014 FC72 is particularly unusual as it has an unusually circular orbit for a scattered-disc object (SDO). Although it is thought that traditional scattered-disc objects have been ejected into their current orbits by gravitational interactions with Neptune, the low eccentricity of its orbit and the distance of its perihelion (SDOs generally have highly eccentric orbits and perihelia less than 38 AU) seems hard to reconcile with such celestial mechanics. This has led to some uncertainty as to the current theoretical understanding of the outer Solar System. The theories include close stellar passages, unseen planet/rogue planets/planetary embryos in the early Kuiper belt, and resonance interaction with an outward-migrating Neptune. The Kozai mechanism is capable of transferring orbital eccentricity to a higher inclination.[10][9]
Physical characteristics
[edit]2014 FC72 has a diameter estimated at around 500 kilometers (310 miles), roughly a fifth the size of Pluto.[5][7]
References
[edit]- ^ a b c d "2014 FC72". Minor Planet Center. Retrieved 12 December 2018.
- ^ a b c d "JPL Small-Body Database Browser: (2014 FC72)" (2017-04-03 last obs.). Jet Propulsion Laboratory. Retrieved 12 December 2018.
- ^ a b Jewitt, David, Morbidelli, Alessandro, & Rauer, Heike. (2007). Trans-Neptunian Objects and Comets: Saas-Fee Advanced Course 35. Swiss Society for Astrophysics and Astronomy. Berlin: Springer. ISBN 3-540-71957-1.
- ^ a b Lykawka, Patryk Sofia; Mukai, Tadashi (July 2007). "Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation". Icarus. 189 (1): 213–232. Bibcode:2007Icar..189..213L. doi:10.1016/j.icarus.2007.01.001.
- ^ a b c d e f Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 12 December 2018.
- ^ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
- ^ a b c Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 12 December 2018.
- ^ "2014 FC72 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site, Department of Mathematics, University of Pisa, Italy. Retrieved 12 December 2018.
- ^ a b Sheppard, Scott S.; Trujillo, Chadwick; Tholen, David J. (July 2016). "Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects with Moderate Semimajor Axes and Eccentricities". The Astrophysical Journal Letters. 825 (1): 7. arXiv:1606.02294. Bibcode:2016ApJ...825L..13S. doi:10.3847/2041-8205/825/1/L13. S2CID 118630570.
- ^ a b Allen, R. L.; Gladman, B.; Kavelaars, J. J.; Petit, J.-M.; Parker, J. W.; Nicholson, P. (March 2006). "Discovery of a Low-Eccentricity, High-Inclination Kuiper Belt Object at 58 AU". The Astrophysical Journal. 640 (1): L83–L86. arXiv:astro-ph/0512430. Bibcode:2006ApJ...640L..83A. doi:10.1086/503098. S2CID 15588453. (Discovery paper)
External links
[edit]- List Of Centaurs and Scattered-Disk Objects, Minor Planet Center
- List of Known Trans-Neptunian Objects, Johnston's Archive
- (690420) 2014 FC72 at AstDyS-2, Asteroids—Dynamic Site
- (690420) 2014 FC72 at the JPL Small-Body Database
