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2014 FZ71

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2014 FZ71
Discovery[1]
Discovered byCTIO
Discovery siteCTIO
(first observed only)
Discovery date24 March 2014
Designations
2014 FZ71
Orbital characteristics[2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 6
Observation arc1.96 yr (716 d)
Aphelion95.791 AU
Perihelion55.849 AU
75.820 AU
Eccentricity0.2634
660.21 yr (241,142 d)
349.80°
0° 0m 5.4s / day
Inclination25.506°
306.01°
244.94°
Physical characteristics
  • 0.08 (assumed)[7]
  • 0.09 (assumed)[5]
24.61[8]
6.9[1][2]

2014 FZ71 is a trans-Neptunian object, a scattered disc 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 a team led by American astronomer Scott Sheppard at the Cerro Tololo Inter-American Observatory in Chile. With its perihelion of almost 56 AU, it belongs to a small and poorly understood group of very distant objects with moderate eccentricities.[6][9] The object is not a dwarf planet candidate as it only measures approximately 150 kilometers (93 miles) in diameter.

Discovery and naming

2014 FZ71 was first observed on 24 March 2014 by a team of astronomers led by Scott Sheppard of the Carnegie Institution for Science as part of the survey for distant solar system objects beyond the Kuiper Cliff using the new wide-field cameras on the Subaru and Cerro Tololo Inter-American Observatory (CTIO) telescopes.[6]

Orbit and classification

The object is located in the "gap", a poorly understood region.

2014 FZ71 orbits the Sun at a distance of 55.8–95.8 AU once every 660 years and 3 months (241,142 days; semi-major axis of 75.82 AU). Its orbit has a moderate eccentricity of 0.26 and an inclination of 26° with respect to the ecliptic.[2]

The object belongs to the same orbital group as 2004 XR190 ("Buffy"), 2014 FC72, 2015 FJ345 and 2015 KQ174 (also see diagram). With an orbital period of 660 years, it seems to be resonant trans-Neptunian objects in a 1:4 resonance with Neptune, as are 2003 LA7 and 2011 UP411,[5] but with a lower eccentricity and therefore higher perihelion.

Considered a scattered and detached object,[3][4][5] 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.[9]

Physical characteristics

2014 FZ71 has a diameter estimated between 125 and 185 kilometers,[6][7][5] roughly a quarter the size of 2004 XR190 ("Buffy") which is estimated at 500 kilometres (310 mi), roughly a quarter the size of Pluto. It is therefore not a dwarf planet candidate.[7]

References

  1. ^ a b c "2014 FZ71". Minor Planet Center. Retrieved 12 December 2018.
  2. ^ a b c d "JPL Small-Body Database Browser: (2014 FZ71)" (2016-03-09 last obs.). Jet Propulsion Laboratory. Retrieved 12 December 2018.
  3. ^ 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.
  4. ^ 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.
  5. ^ 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.
  6. ^ a b c d 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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  7. ^ a b c d Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 12 December 2018.
  8. ^ "2014 FZ71 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site, Department of Mathematics, University of Pisa, Italy. Retrieved 12 December 2018.
  9. ^ 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)
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