(523635) 2010 DN93
DiscoveryMPO 450766 | |
---|---|
Discovered by |
first observed by: Pan-STARRS 1 |
Discovery date | 26 February 2010 |
Designations | |
MPC designation | (523635) 2010 DN93 |
distant[1] · TNO[2] · cubewano · detached | |
Orbital characteristics [2] | |
Epoch 23 March 2018 (JD 2458200.5) | |
Uncertainty parameter 1 | |
Observation arc | 15.17 yr (5,541 days) |
Aphelion | 65.888 AU |
Perihelion | 45.099 AU |
55.494 AU | |
Eccentricity | 0.187 |
413 yr (150,745 days) | |
39.73° | |
0° 0m 8.64s / day | |
Inclination | 40.597° |
91.26° | |
32.99° | |
Physical characteristics | |
Dimensions | 500 km[1] |
21.9[3] | |
4.8[1] | |
|
(523635) 2010 DN93 is a trans-Neptunian object, located in the scattered disc, the outermost region of the Solar System.[4] It orbits the Sun in a moderate inclined, moderate-eccentricity orbit. The object was discovered in February 2010.
Discovery and naming
(523635) 2010 DN93 was discovered on 26 February 2010. It was discovered at Pan-STARRS 1.
Orbit
Considered a detached object,[5][6] (523635) 2010 DN93 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]. It is in a 5:2 resonance to Neptune. It seems to belong to the same group as (145480) 2005 TB190.
Size
(523635) 2010 DN93 has a diameter estimated at around 500 kilometres (310 mi), roughly a quarter the size of Pluto, and it orbits between 45 and 66 AU from the Sun.
References
- 1 2 3 "2010 DN93". Minor Planet Center. Retrieved 2018-10-12.
- 1 2 "JPL Small-Body Database Browser: 2010 DN93" (2015-01-24 last obs.). Jet Propulsion Laboratory. Retrieved 28 February 2017.
- ↑ "AstDys 2010 DN93 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2018-10-12.
- ↑ 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)
- ↑ 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.
- ↑ 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.
- ↑ 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)