(523635) 2010 DN93

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(523635) 2010 DN93
Discovery [1] [2]
Discovered by Pan-STARRS 1
Discovery site Haleakala Obs.
Discovery date26 February 2010
Designations
(523635) 2010 DN93
2010 DN93
TNO [3]  · SDO [4] [5]
detached [6] [7]  · distant [1]
Orbital characteristics [3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 3
Observation arc 15.17 yr (5,541 d)
Aphelion 65.507 AU
Perihelion 45.066 AU
55.287 AU
Eccentricity 0.1849
411.09 yr (150,152 d)
41.383°
0° 0m 8.64s / day
Inclination 40.598°
91.306°
32.315°
Physical characteristics
Mean diameter
486  km (est.) [4]
490  km (est.) [8]
0.07 (est.) [8]
0.09 (est.) [4]
21.82 [9]
4.8 [1] [3]
5.1 [8]

    (523635) 2010 DN93 (provisional designation 2010 DN93) is a trans-Neptunian object from in the scattered disc located in the outermost region of the Solar System. It was discovered on 26 February 2010, by astronomers with the Pan-STARRS survey at Haleakala Observatory on the island of Maui, Hawaii, in the United States. [1] Assuming a low albedo, the object is estimated at approximately 490 kilometers (300 miles) in diameter. [4] It was numbered in 2018 and remains unnamed.

    Contents

    Orbit and classification

    (523635) 2010 DN93 is located near the "gap", a poorly understood region. Extreme transneptunian object eccentricity vs perihelion.png
    (523635) 2010 DN93 is located near the "gap", a poorly understood region.

    2010 DN93 orbits the Sun at a distance of 45.1–65.5  AU once every 411 years (150,152 days; semi-major axis of 55.29 AU). Its orbit has an eccentricity of 0.18 and an inclination of 41° with respect to the ecliptic. [3]

    This distant minor planet is a trans-Neptunian object and a member of the scattered disc population. [3] [4] 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.

    2010 DN93 has also been considered a detached object, [6] [7] since its relatively low eccentricity of 0.18, and its perihelion distance of 45.1 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. [10] [11] 2010 DN93 seems to belong to the same group as 2005 TB190 .

    Numbering and naming

    The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey at Apache Point Observatory in March 2003, almost seven years prior to its official discovery observation at Haleakala. [1] It was numbered by the Minor Planet Center on 25 September 2018 ( M.P.C. 111778). [12] As of 2018, it has not been named. [1]

    Physical characteristics

    Diameter and albedo

    2010 DN93 has an absolute magnitude of 4.8. [1] According to the Johnston's archive and astronomer Michael Brown, it measures 486 and 490 kilometers in diameter, based on an assumed albedo for the body's surface of 0.09 and 0.07, respectively. [4] [8] As of 2018, no physical characteristics have been determined from photometric observations. The body's color, rotation period, pole and shape remain unknown. [3] [13]

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    References

    1. 1 2 3 4 5 6 7 "523635 (2010 DN93)". Minor Planet Center. Retrieved 18 October 2018.
    2. ↑ Gibson, B.; Goggia, T.; Primak, N.; Schultz, A.; Willman, M.; Chen, Y.-T.; et al. (July 2016). "2010 DN93". Minor Planet Electronic Circ. 2016-O308 (2016–O308 (2016)). Bibcode:2016MPEC....O..308G . Retrieved 18 October 2018.
    3. 1 2 3 4 5 6 "JPL Small-Body Database Browser: 523635 (2010 DN93)" (2018-05-25 last obs.). Jet Propulsion Laboratory . Retrieved 18 October 2018.
    4. 1 2 3 4 5 6 Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 18 October 2018.
    5. ↑ "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 18 October 2018.
    6. 1 2 Jewitt, D; A, Morbidelli; H, Rauer; K, Altwegg; W, Benz; N, Thomas (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.
    7. 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.
    8. 1 2 3 4 Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 18 October 2018.
    9. ↑ "Asteroid (523635) 2010 DN93". AstDyS-2, Asteroids – Dynamic Site, University of Pisa, Italy. Retrieved 18 October 2018.
    10. ↑ 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. (Discovery paper)
    11. ↑ 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)
    12. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 18 October 2018.
    13. ↑ "LCDB Data for (523635)". Asteroid Lightcurve Database (LCDB). Retrieved 18 October 2018.
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