(82075) 2000 YW134

(82075) 2000 YW134
Discovered bySpacewatch
Discovery siteKitt Peak National Obs.
Discovery date26 December 2000
(82075) 2000 YW134
2000 YW134 · 2001 XG201[3]
TNO[4] · res (3:8)[5][6]
Orbital characteristics[4]
Epoch 1 July 2021 (JD 2459396.5)
Uncertainty parameter 2[2][4]
Observation arc20.19 yr (7,373 d)
Aphelion73.783 AU
Perihelion40.999 AU
57.391 AU
434.78 yr (158,805 d)
0° 0m 8.28s / day
Known satellitesS/2005 (82075) 1
(Ds/Dp: 0.347)[7]
Physical characteristics
Mean diameter

(82075) 2000 YW134, provisional designation: 2000 YW134, is a resonant trans-Neptunian object and binary system, located in the outermost region of the Solar System. It was discovered on 26 December 2000, by astronomers with the Spacewatch survey at Kitt Peak Observatory near Tucson, Arizona. The reddish object stays in a rare 3:8 resonance with Neptune and measures approximately 216 kilometers (130 miles). Its 75-kilometer sized companion was discovered by the Hubble Space Telescope in October 2002.[7] As of 2021, neither the primary body nor its satellite have been named.[2]

Orbit and classification[]

2000 YW134 orbits the Sun at a distance of 41.0–73.8 AU once every 434 years and 9 months (158,805 days; semi-major axis of 57.39 AU). Its orbit has an eccentricity of 0.29 and an inclination of 20° with respect to the ecliptic.[4] The body's observation arc begins with its official discovery observation by Spacewatch on 26 December 2000.[2] It last came to perihelion in 1979,[12] and is currently at about 46.5 AU from the Sun, with an apparent magnitude of 21.54.[11] It will reach aphelion in December 2197.[12]

2000 YW134 is a resonant trans-Neptunian object that stays in a rare 3:8 mean-motion orbital resonance with Neptune, orbiting exactly three times the Sun for every 8 orbits Neptune does.[6] There are currently two other objects known to have the same resonant type: 2014 UE228 and (542258) 2013 AP183.[5][13] Due to its relatively large distance to Neptune, a classification as an extended-scattered or detached object was also considered earlier on (Lykawka, 2006). However, improved observations and long-term numerical integrations of the object's orbit by Emel’yanenko and Kiseleva (84% probability) and the Deep Ecliptic Survey – with all alternative integrations in agreement, showing a minimum perihelion distance of 38.2 AU – have since secured its 3:8 orbital resonance with Neptune.[6][14]

Numbering and naming[]

This minor planet was numbered by the Minor Planet Center on 4 May 2004, receiving the number (82075) in the minor planet catalog (M.P.C. 51853).[15] As of 2021, it has not been named.[2] According to the established naming conventions, it will be given a mythological name associated with the underworld.[16]

Physical characteristics[]

The surface of 2000 YW134 is moderately red in the visible part of the spectrum. Its IR spectral type transitions from the very red (RR) to the intermediate blue-red (BR).[10] Alternatively a BR-spectral type has also been assumed.[7] The object's B−V and V–R color indices have also been measured several times, giving an averaged value of close to 1.0 and 0.5, respectively, for a combined B−R magnitude of 1.50.[9]

Diameter and albedo[]

In 2010, observations with the Herschel Space Observatory constrained the object's geometric albedo to no darker than 8%, and allowed to place an upper limit to its effective mean-diameter of 500 km (310 mi), as no thermal radiation had been detected.[8] However, according to Michael Mommert's dissertation in 2013, the object has a much higher albedo of 0.408±0.329, which greatly reduces its effective diameter to 229 km (140 mi).[7]


On 25 October 2002, observations in the far-infrared with the NICMOS instrument of the Hubble Space Telescope revealed, that 2000 YW134 is a binary system with a satelite in its orbit. The discovery was announced on 6 October 2005.[7][17]: 22 Johnston's Archive derives a diameter of 216 km (130 mi) for the primary and a diameter of 75 km (47 mi) for the secondary, based on a secondary-to-primary diameter ratio of 0.347, for a difference of 1.3 magnitudes between the two objects. The satellite, designated S/2005 (82075) 1, orbits its primary every 10 days (estimated) at an average distance of 1,900 km (1,200 mi).[7]


  1. ^ "MPEC 2001-B03 : 2000 YW134". Minor Planet Electronic Circular. Minor Planet Center. 16 January 2001. Retrieved 9 September 2021.
  2. ^ a b c d e f "82075 (2000 YW134)". Minor Planet Center. Retrieved 9 September 2021.
  3. ^ "MPEC 2002-A26 : 2000 YW134 = 2001 XG201". Minor Planet Electronic Circular. Minor Planet Center. 7 January 2002. Retrieved 9 September 2021.
  4. ^ a b c d e "JPL Small-Body Database Browser: 82075 (2000 YW134)" (2021-03-04 last obs.). Jet Propulsion Laboratory. Retrieved 9 September 2021.
  5. ^ a b c d "List of Known Trans-Neptunian Objects". Johnston's Archive. 18 August 2020. Retrieved 9 September 2021.
  6. ^ a b c "Orbit Fit and Astrometric record for 82075". Southwest Research Institute. Retrieved 9 September 2021.
  7. ^ a b c d e f g h i j Johnston, Wm. Robert (20 September 2014). "Asteroids with Satellites Database – (82075) 2000 YW134". Johnston's Archive. Retrieved 9 September 2021. Mommert, M., 2013, p.164 and Grundy, 2012
  8. ^ a b Müller, T. G.; Lellouch, E.; Stansberry, J.; Kiss, C.; Santos-Sanz, P.; Vilenius, E.; et al. (July 2010). "TNOs are Cool: A survey of the trans-Neptunian region. I. Results from the Herschel science demonstration phase (SDP)". Astronomy and Astrophysics. 518: L146. arXiv:1005.2923. Bibcode:2010A&A...518L.146M. doi:10.1051/0004-6361/201014683. ISSN 0004-6361. S2CID 118635387.
  9. ^ a b c d "LCDB Data for (82075)". Asteroid Lightcurve Database (LCDB). Retrieved 9 September 2021.
  10. ^ a b 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. ISSN 0019-1035.
  11. ^ a b "Asteroid (82075) 2000 YW134 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site. Retrieved 9 September 2021.
  12. ^ a b "Horizon Online Ephemeris System". California Institute of Technology, Jet Propulsion Laboratory. Retrieved 8 September 2021.
  13. ^ "The Deep Ecliptic Survey Object Classifications". Southwest Research Institute. Retrieved 9 September 2021.
  14. ^ 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. ISSN 0320-0108. S2CID 122634598.
  15. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 9 September 2021.
  16. ^ "Naming of Astronomical Objects – Minor planets". IAU – International Astronomical Union. Retrieved 27 July 2021.
  17. ^ Stephens, Denise C.; Noll, Keith S. (February 2006). "Detection of Six Trans-Neptunian Binaries with NICMOS: A High Fraction of Binaries in the Cold Classical Disk". The Astronomical Journal. 131 (2): 1142–1148. arXiv:astro-ph/0510130. Bibcode:2006AJ....131.1142S. doi:10.1086/498715. ISSN 0004-6256.

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