astro.wikisort.org - Asteroid

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.

2015 KQ₁₇₄

Discovery[1]
Discovered by	Mauna Kea Obs.
Discovery site	Mauna Kea Obs. (first observed only)
Discovery date	24 May 2015
Designations
MPC designation	2015 KQ174
Minor planet category	TNO[2] detached[3][4] SDO[5] distant[1]
Orbital characteristics[2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 4
Observation arc	3.24 yr (1,183 d)
Aphelion	61.483 AU
Perihelion	49.311 AU
Semi-major axis	55.397 AU
Eccentricity	0.1099
Orbital period (sidereal)	412.32 yr (150,600 d)
Mean anomaly	76.743°
Mean motion	0° 0m 8.64s / day
Inclination	24.344°
Longitude of ascending node	213.92°
Argument of perihelion	294.05°
Physical characteristics
Mean diameter	154 km[5]
Geometric albedo	0.09 (assumed)[5]
Apparent magnitude	25.01[6]
Absolute magnitude (H)	7.3[1][2]

Orbit and classification

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

External links

• List Of Centaurs and Scattered-Disk Objects, Minor Planet Center
• List of Known Trans-Neptunian Objects, Johnston's Archive
• 2015 KQ174 at AstDyS-2, Asteroids—Dynamic Site
  • Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• 2015 KQ174 at the JPL Small-Body Database
  • Close approach · Discovery · Ephemeris · Orbit diagram · Orbital elements · Physical parameters

На других языках

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[de] 2015 KQ174

2015 KQ174 ist ein Planetoid, der am 24. Mai 2015 am Mauna Kea entdeckt wurde und zur Gruppe der Kuipergürtel-Planetoiden gehört. Der Asteroid läuft auf einer mäßig exzentrischen Bahn in 503 Jahren um die Sonne, sodass er sich in einer 5:2-Bahnresonanz mit dem Neptun befindet. Die Bahnexzentrizität seiner Bahn beträgt 0,11, wobei diese 24,34° gegen die Ekliptik geneigt ist.[1]

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- [en] 2015 KQ174

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