(690420) 2014 FC72

Trans-Neptunian object 2014 FE 72 and 2014 FZ 71 October 2018 yes (690420) 2014 FC 72 #C2E0FF Pan-STARRS 1 Haleakala Obs. 24 March 2014(first observed only) (690420) 2014 FC 72 TNO detached SDO distant 27 April 2019 (JD 2458600.5) 3 16.91 yr (6,178 d) 100.57 AU 51.663 AU ≈ 25 November 2023JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)±7 days 76.114 AU 0.3212 664.06 yr (242,547 d) 357.23° 0.0015 ms / day 29.859° 178.00° 33.138° 0 431 km 506 km 0.07 (assumed) 0.124 (assumed) 22.09 4.684.70 (690420) 2014 FC 72 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. With its perihelion distant from Neptune, it belongs to a small and poorly understood group of objects with moderate eccentricities. It is estimated to measure 400 to 500 km mi off 1 us in diameter, assuming a low albedo. Orbit and classification thumb|left|200px|The object is located in the "gap", a poorly understood region. 2014 FC 72 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. The object belongs to the same orbital group as (612911) 2004 XR 190 ("Buffy"), 2014 FZ 71, 2015 FJ 345 and 2015 KQ 174 (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 LA 7 and 2011 UP 411, but with lower eccentricities and therefore higher perihelia as the latter. Considered a scattered and detached object, 2014 FC 72 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. Physical characteristics 2014 FC 72 has a diameter estimated at 400 to 500 km mi off us, making it approximately 18% to 21% the size of the dwarf planet Pluto.Pluto Pluto has a diameter of 2376.6 km mi. 18% and 21% of Pluto's diameter is 428 km mi and 499 km mi, which is roughly around 2014 FC 72's size of 431 km to 506 km. With Johnston's Archive's estimate being 431 km mi off 3 us, and Mike Brown's estimate being 506 km mi off 3 us, assuming albedos of 0.124 and 0.07, respectively. However, Mike Brown's estimate uses an outdated absolute magnitude of 5.0, not the newer 4.68 nor 4.70. Notes References 30em 2017-04-03 last obs. JPL Small-Body Database Browser: (2014 FC72) https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=3755688 Jet Propulsion Laboratory 12 December 2018 2014 FC72 Minor Planet Center https://www.minorplanetcenter.net/db_search/show_object?object_id=2014+FC72 12 December 2018 List of Known Trans-Neptunian Objects Johnston's Archive 5 September 2026 Johnston Wm. Robert http://www.johnstonsarchive.net/astro/tnoslist.html 12 December 2018 How many dwarf planets are there in the outer solar system? California Institute of Technology Brown Michael E. http://web.gps.caltech.edu/~mbrown/dps.html 12 December 2018 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. 3-540-71957-1. Patryk Sofia Lykawka Tadashi Mukai July 2007 Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation Icarus 189 1 213–232 2007Icar..189..213L 10.1016/j.icarus.2007.01.001 R. L. Allen B. Gladman J. J. Kavelaars J.-M. Petit J. W. Parker P. Nicholson March 2006 Discovery of a Low-Eccentricity, High-Inclination Kuiper Belt Object at 58 AU The Astrophysical Journal 640 1 L83–L86 2006ApJ...640L..83A 10.1086/503098 astro-ph/0512430 15588453 (Discovery paper) Scott S. Sheppard Chadwick Trujillo David J. Tholen 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 2016ApJ...825L..13S 10.3847/2041-8205/825/1/L13 1606.02294 118630570 free 2014 FC72 – Ephemerides AstDyS-2, Asteroids Dynamic Site, Department of Mathematics, University of Pisa, Italy https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=2014FC72 12 December 2018 Nimmo Francis etal Mean radius and shape of Pluto and Charon from New Horizons images Icarus 2017 287 12–29 2017Icar..287...12N 1603.00821 10.1016/j.icarus.2016.06.027 External links List Of Centaurs and Scattered-Disk Objects, Minor Planet Center List of Known Trans-Neptunian Objects, Johnston's Archive 2014FC72 3755688 690420 (690420) 2014 FC 72 Category:Scattered disc and detached objects Category:Discoveries by Pan-STARRS 20140324 Category:Trans-Neptunian objects in a 1:4 resonance