2014 FC72
DiscoveryMPO 456887 | |
---|---|
Discovered by |
first observed by: Pan-STARRS 1, Haleakala |
Discovery date | 24 March 2014 |
Designations | |
MPC designation | 2014 FC72 |
distant[1] · TNO[2] · cubewano · detached | |
Orbital characteristics [2] | |
Epoch 23 March 2018 (JD 2458200.5) | |
Uncertainty parameter 1 | |
Observation arc | 16.91 yr (6,178 days) |
Aphelion | 101.005 AU |
Perihelion | 51.671 AU |
76.338 AU | |
Eccentricity | 0.3231 |
667 yr (247,835 days) | |
356.81° | |
0° 0m 5.4s / day | |
Inclination | 29.825° |
177.96° | |
32.84° | |
Physical characteristics | |
Dimensions | 400–500 km[3] |
22.03[4] | |
4.7[1] | |
|
2014 FC72 is a trans-Neptunian object and possible dwarf planet, located in the scattered disc, the outermost region of the Solar System.[3] It orbits the Sun in a moderate inclined, moderate-eccentricity orbit. The object was discovered in March 2014.
Discovery and naming
2014 FC72 was discovered on 24 March 2014. It was discovered at Pan-STARRS 1, Haleakala.
Orbit
Considered a detached object,[5][6] 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.[7] As 2014 FZ71 it is in a 4:1 resonance to Neptune. It seems to belong to the same group as 2004 XR190.
Size
2014 FC72 has a diameter estimated at around 500 kilometres (310 mi), roughly a fifth the size of Pluto, and it orbits between 51 and 101 AU from the Sun.
References
- 1 2 "2014 FC72". Minor Planet Center. Retrieved 2018-10-09.
- 1 2 "JPL Small-Body Database Browser: 2014 FC72" (2015-01-24 last obs.). Jet Propulsion Laboratory. Retrieved 28 February 2017.
- 1 2 Scott. S. Sheppard; Chadwick Trujillo; David J. Tholen (2015). "Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects With Moderate Semi-major Axes and Eccentricities". The Astrophysical Journal Letters. 825/1: L13. arXiv:1606.02294. Bibcode:2006ApJ...640L..83A. doi:10.3847/2041-8205. (Discovery paper)
- ↑ "AstDys 2014 FC72 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2018-10-09.
- ↑ 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.
- ↑ Lykawka, Patryk Sofia & Mukai, Tadashi. (2007). Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation. Icarus Volume 189, Issue 1, July, Pages 213–232. doi:10.1016/j.icarus.2007.01.001.
- ↑ R. L. Allen; B. Gladman (2006). "Discovery of a low-eccentricity, high-inclination Kuiper belt object at 58 AU". The Astrophysical Journal. 640: L83. arXiv:astro-ph/0512430. Bibcode:2006ApJ...640L..83A. doi:10.1086/503098. (Discovery paper)