Astronomy:(533560) 2014 JM80

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(533560) 2014 JM80
Discovery[1]
Discovered byPan-STARRS 1
Discovery siteHaleakala Obs.
Discovery date9 May 2010
Designations
(533560) 2014 JM80
2014 JM80
Minor planet categoryTNO[2] · SDO[3][4]
distant[1]
Orbital characteristics[2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 4
Observation arc2.93 yr (1,070 d)
|{{{apsis}}}|helion}}80.184 AU
|{{{apsis}}}|helion}}45.965 AU
63.074 AU
Eccentricity0.2713
Orbital period500.94 yr (182,969 d)
Mean anomaly343.18°
Mean motion0° 0m 7.2s / day
Inclination20.479°
Longitude of ascending node182.43°
|{{{apsis}}}|helion}}≈ 20 November 2042[5]
±8 days
96.342°
Physical characteristics
Mean diameter329 km[6]
352 km[3]
Absolute magnitude (H)5.5[1][2]


(533560) 2014 JM80, provisional designation 2014 JM80, is a trans-Neptunian object from the scattered disc in the outermost Solar System, approximately 340 kilometers (210 miles) in diameter. It was discovered on 9 May 2010 by astronomers with the Pan-STARRS-1 survey at the Haleakala Observatory, Hawaii, in the United States.[1] According to American astronomer Michael Brown, it is "possibly" a dwarf planet.[3][6]

Orbit and classification

2014 JM80 is located near the "gap", a poorly understood region.

2014 JM80 orbits the Sun at a distance of 46.0–80.2 AU once every 500 years and 11 months (182,969 days; semi-major axis of 63.07 AU). Its orbit has an eccentricity of 0.27 and an inclination of 20° with respect to the ecliptic.[2]

This distant minor planet is a trans-Neptunian object and a member of the scattered disc population. Scattered-disc objects are thought to have been ejected from the classical Kuiper belt into their current orbits by gravitational interactions with Neptune, and typically have highly eccentric orbits and perihelia of less than 38 AU.

2014 JM80 has also been considered a detached object,[7][8] since its relatively low eccentricity of 0.27, and its perihelion distance of 46.0 AU are hard to reconcile with the celestial mechanics of a scattered-disc object. This has led to some uncertainty as to the current theoretical understanding of the outermost 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][10]

With an orbital period of 500 years, and similar to 2015 FJ345, it seems to be a resonant trans-Neptunian objects in a 1:3 resonance with Neptune,[9]:12 as several other objects, but with a lower eccentricity (0.27 instead of more than 0.60) and a higher perihelia (at 45.8 AU rather than 31–41 AU). 2014 JM80 seems to belong to the same group as 2005 TB190.

References

  1. ↑ 1.0 1.1 1.2 1.3 "2014 JM80". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=2014+JM80. Retrieved 9 October 2018. 
  2. ↑ 2.0 2.1 2.2 2.3 "JPL Small-Body Database Browser: (2014 JM80)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=3755645. Retrieved 9 October 2018. 
  3. ↑ 3.0 3.1 3.2 Johnston, Wm. Robert (30 December 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. http://www.johnstonsarchive.net/astro/tnoslist.html. Retrieved 9 February 2018. 
  4. ↑ "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. https://www.minorplanetcenter.net/iau/lists/t_centaurs.html. Retrieved 9 February 2018. 
  5. ↑ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
  6. ↑ 6.0 6.1 Brown, Michael E.. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. http://web.gps.caltech.edu/~mbrown/dps.html. Retrieved 9 February 2018. 
  7. ↑ Jewitt, D; A, Morbidelli; H, Rauer (2008). Trans-Neptunian objects and comets : Saas-Fee Advanced Course 35. Swiss society for astrophysics and astronomy. Berlin New York: Springer. p. 86. ISBN 978-3-540-71957-1. OCLC 261225528. https://archive.org/details/transneptunianob00jewi. 
  8. ↑ Lykawka, Patryk Sofia; Mukai, Tadashi (July 2007). "Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation". Icarus 189 (1): 213–232. doi:10.1016/j.icarus.2007.01.001. Bibcode: 2007Icar..189..213L. 
  9. ↑ 9.0 9.1 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. doi:10.3847/2041-8205/825/1/L13. Bibcode: 2016ApJ...825L..13S.  (Discovery paper)
  10. ↑ 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. doi:10.1086/503098. Bibcode: 2006ApJ...640L..83A.  (Discovery paper)

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