(48639) 1995 TL8
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48639 1995 TL8
Discovery [1][2]
Discovered byA. Gleason (Spacewatch)
Discovery site
Discovery date15 October 1995
MPC designation
TNO[1] · SDO[3]
detached[4] · distant[2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 2
Observation arc19.30 yr (7,049 days)
Aphelion64.486 AU
Perihelion39.969 AU
52.227 AU
377.45 yr (137,863 days)
0° 0m 9.36s / day
Known satellites1 (D: 80 km)[5]
Physical characteristics
Dimensions176 km[5]
420.27 km (calculated)[6]
495 km (estimated)[7]
0.07 (estimated)[7]
0.10 (assumed)[6]
RR[8] · C (assumed)[6]
(R)[9] · 5.0[1][6] · 5.1[7] · [a]

is a binary trans-Neptunian object from the scattered disc in the outermost regions of the Solar System. It was discovered by Arianna Gleason in 1995 and measures approximately 176 kilometers in diameter. Its 80-kilometer minor-planet moon, provisionally designated , was discovered on 9 November 2002.[5]


was discovered on 15 October 1995, by American astronomer Arianna Gleason as part of UA's Spacewatch survey at Kitt Peak National Observatory, near Tucson, Arizona.[2]

It was the first of the bodies presently classified as a scattered-disc object (SDO)[3] to be discovered, preceding the SDO prototype by almost a year.[]


A companion was discovered by Denise C. Stephens and Keith S. Noll, from observations with the Hubble Space Telescope taken on 9 November 2002, and announced on 5 October 2005. The satellite, designated , is relatively large, having a likely mass of about 10% of the primary. Its orbit has not been determined, but it was at a separation of only about 420 kilometres (260 mi) to the primary at the time of discovery, with a possible orbital period of about half a day and an estimated diameter of 161 kilometres (100 mi).[5]

A relative size and distance comparison of the system with the Earth-Moon system. The scale of the Earth-Moon system has been reduced so Earth appears the same size as the primary.

Scattered-extended object

is classified as detached object (scattered-extended) by the Deep Ecliptic Survey, since its orbit appears to be beyond significant gravitational interactions with Neptune's current orbit.[4] However, if Neptune migrated outward, there would have been a period when Neptune had a higher eccentricity.

Simulations made in 2007 show that appears to have less than a 1% chance of being in a 3:7 resonance with Neptune, but it does execute circulations near this resonance.[10]

Left: The near 3:7 resonance pattern of with Neptune only moves clockwise. It never halts and reverses course (i.e. librates).
Right: The orbital period of missing the 7:3 (2.333) resonance of Neptune

Numbering and naming

This minor planet was numbered by the Minor Planet Center on 20 November 2002.[11] As of 2018, it has not been named.[2]

See also

  • 3753 Cruithne (orbital circulations due to near resonant perturbations with Earth)
  • - to see a proper 3:7 resonance with Neptune


  1. ^ Lellouch (2013): observations on 11 February 2011 gave an absolute magnitude of . Summary figures for (48639) at LCDB not found at ADS (2013A&A...557...60L)


  1. ^ a b c d "JPL Small-Body Database Browser: 48639 (1995 TL8)" (2015-02-01 last obs.). Jet Propulsion Laboratory. Retrieved 2017.
  2. ^ a b c d "48639 (1995 TL8)". Minor Planet Center. Retrieved 2017.
  3. ^ a b Johnston, Wm. Robert (15 October 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 2017.
  4. ^ a b Marc W. Buie (22 October 2003). "Orbit Fit and Astrometric record for 48639". SwRI (Space Science Department). Retrieved 2009.
  5. ^ a b c d e Johnston, Wm. Robert (21 September 2014). "Asteroids with Satellites Database - (48639) 1995 TL8". Johnston's Archive. Retrieved 2017.
  6. ^ a b c d "LCDB Data for (48639)". Asteroid Lightcurve Database (LCDB). Retrieved 2017.
  7. ^ a b c Michael E. Brown. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 2017.
  8. ^ Belskaya, Irina N.; Barucci, Maria A.; Fulchignoni, Marcello; Dovgopol, Anatolij N. (April 2015). "Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo". Icarus. 250: 482-491. Bibcode:2015Icar..250..482B. doi:10.1016/j.icarus.2014.12.004. Retrieved 2016.
  9. ^ Peixinho, N.; Delsanti, A.; Guilbert-Lepoutre, A.; Gafeira, R.; Lacerda, P. (October 2012). "The bimodal colors of Centaurs and small Kuiper belt objects". Astronomy and Astrophysics. 546: 12. arXiv:1206.3153. Bibcode:2012A&A...546A..86P. doi:10.1051/0004-6361/201219057. Retrieved 2017.
  10. ^ Emel'Yanenko, V. V.; Kiseleva, E. L. (April 2008). "Resonant motion of trans-Neptunian objects in high-eccentricity orbits". Astronomy Letters. 34 (4): 271-279. Bibcode:2008AstL...34..271E. doi:10.1134/S1063773708040075. Retrieved 2017.
  11. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 2018.

External links

  This article uses material from the Wikipedia page available here. It is released under the Creative Commons Attribution-Share-Alike License 3.0.



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