2015 KQ174
Discovery[1]
Discovered byMauna Kea Obs.
Discovery siteMauna Kea Obs.
(first observed only)
Discovery date24 May 2015
Designations
2015 KQ174
Orbital characteristics[2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 4
Observation arc3.24 yr (1,183 d)
Aphelion61.483 AU
Perihelion49.311 AU
55.397 AU
Eccentricity0.1099
412.32 yr (150,600 d)
76.743°
0° 0m 8.64s / day
Inclination24.344°
213.92°
294.05°
Physical characteristics
Mean diameter
154 km[5]
0.09 (assumed)[5]
25.01[6]
7.3[1][2]

    2015 KQ174 is a trans-Neptunian object, both considered a scattered and detached object, located in the outermost region of the Solar System. The object with a moderately inclined and eccentric orbit measures approximately 154 kilometers (96 miles) in diameter. It was first observed on 24 May 2015, by astronomers at the Mauna Kea Observatories in Hawaii, United States.

    Orbit and classification

    2015 KQ174 is located near the "gap", a poorly understood region.

    2015 KQ174 orbits the Sun at a distance of 49.3–61.5 AU once every 412 years and 4 months (150,600 days; semi-major axis of 55.4 AU). Its orbit has an eccentricity of 0.11 and an inclination of 24° with respect to the ecliptic.[2]

    The object belongs to the same group as 2004 XR190 ("Buffy"), 2014 FC72, 2014 FZ71 and 2015 FJ345 (also see diagram). With an orbital period of 412 years, it seems to be a resonant trans-Neptunian objects in a 2:5 resonance with Neptune,[7]: 12  as several other objects,[5] but with a lower eccentricity (0.11 instead of more than 0.60) and higher perihelia (at 49.3 AU rather than 31–41 AU).

    Considered both a scattered and detached object,[3][4][5] 2015 KQ174 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.[8][7] It is in a 5:2 resonance to Neptune. It seems to belong to the same group as 2004 XR190, nicknamed "Buffy".

    Physical characteristics

    Johnston's archive estimates a diameter of 154 kilometers based on an assumed albedo of 0.09.[5] This is approximately a quarter the size of "Buffy" which is estimated at around 500 kilometres (310 mi), roughly a quarter the size of Pluto.

    References

    1. 1 2 3 "2015 KQ174". Minor Planet Center. Retrieved 13 December 2018.
    2. 1 2 3 4 "JPL Small-Body Database Browser: (2015 KQ174)" (2017-08-24 last obs.). Jet Propulsion Laboratory. Retrieved 13 December 2018.
    3. 1 2 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. 1 2 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. Retrieved 12 December 2018.
    5. 1 2 3 4 5 6 Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 12 December 2018.
    6. ↑ "2015 KQ174 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site, Department of Mathematics, University of Pisa, Italy. Retrieved 12 December 2018.
    7. 1 2 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.
    8. ↑ 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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