astro.wikisort.org - Asteroid

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.

2014 FC₇₂

Discovery[1]
Discovered by	Pan-STARRS 1
Discovery site	Haleakala Obs.
Discovery date	24 March 2014 (first observed only)
Designations
MPC designation	2014 FC72
Minor planet category	TNO[2] detached[3][4] SDO[5] distant[1]
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
Semi-major axis	76.114 AU
Eccentricity	0.3212
Orbital period (sidereal)	664.06 yr (242,547 d)
Mean anomaly	357.23°
Mean motion	0° 0m 5.4s / day
Inclination	29.859°
Longitude of ascending node	178.00°
Time of perihelion	≈ 25 November 2023[6] ±7 days
Argument of perihelion	33.138°
Physical characteristics
Mean diameter	502 km[5] 513 km[7]
Geometric albedo	0.08 (assumed)[7] 0.09 (assumed)[5]
Apparent magnitude	22.09[8]
Absolute magnitude (H)	4.7[1][2]

Orbit and classification

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

2014 FC₇₂ has a diameter estimated at around 500 kilometers (310 miles), roughly a fifth the size of Pluto.[5][7]

References

External links

• List Of Centaurs and Scattered-Disk Objects, Minor Planet Center
• List of Known Trans-Neptunian Objects, Johnston's Archive
• 2014 FC72 at AstDyS-2, Asteroids—Dynamic Site
  • Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• 2014 FC72 at the JPL Small-Body Database
  • Close approach · Discovery · Ephemeris · Orbit diagram · Orbital elements · Physical parameters

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