2014 FZ71

2014 FZ71
DiscoveryMPO 380710
Discovered by first observed by:
Cerro Tololo Observatory, La Serena
Discovery date 24 March 2014
Designations
MPC designation 2014 FZ71
distant[1] · TNO[2] · cubewano · detached
Orbital characteristics [2]
Epoch 27 April 2019 (JD 2458200.5)
Uncertainty parameter 5
Observation arc 1.96 yr (716 days)
Aphelion 95.644 AU
Perihelion 55.881 AU
75.763 AU
Eccentricity 0.2624
659 yr (240,535 days)
350.02°
0° 0m 5.4s / day
Inclination 25.506°
306.01°
244.50°
Physical characteristics
Dimensions 100–150 km[3]
24.61[4]
6.9[1]

    2014 FZ71 is a trans-Neptunian object, 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, by a team of researches led by American astronomer Scott S. Sheppard of the Carnegie Institution for Science.

    Discovery and naming

    2014 FZ71 was discovered on 24 March 2014. It was discovered by astronomers led by Scott Sheppard of the Carnegie Institution for Science as part of the survey for distant solar system objects beyond the Kuiper Belt edge using the new wide-field cameras on the Subaru and Cerro Tololo Inter-American Observatory (CTIO) telescopes.

    Orbit

    Considered a detached object,[5][6] 2014 FZ71 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 FC72 it is in a 4:1 resonance to Neptune. It seems to belong to the same group as 2004 XR190.

    Size

    2014 FZ71 has a diameter estimated at around 150 kilometres (93 mi), roughly a quarter the size of 2004 XR190 which is estimated at around 500 kilometres (310 mi), roughly a quarter the size of Pluto, and it orbits between 55 and 96 AU from the Sun.

    References

    1. 1 2 "2014 FZ71". Minor Planet Center. Retrieved 2018-10-09.
    2. 1 2 "JPL Small-Body Database Browser: 2014 FZ71" (2015-01-24 last obs.). Jet Propulsion Laboratory. Retrieved 28 February 2017.
    3. 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)
    4. ↑ {{cite web ytitle=AstDys 2014 FZ71 Ephemerides epublisher=Department of Mathematics, University of Pisa, Italy ourl= http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.0&n=2014FZ71 caccessdate=2018-10-09
    5. ↑ 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.
    6. ↑ 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.
    7. ↑ 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)

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