(82158) 2001 FP185

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
(82158) 2001 FP185
Discovery [1][2]
Discovered by M. W. Buie
Discovery site Kitt Peak National Obs.
Discovery date 26 March 2001
MPC designation (82158) 2001 FP185
2001 FP185
TNO[1] · SDO[3] · distant[2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 2
Observation arc 16.25 yr (5,937 days)
Aphelion 420.18 AU
Perihelion 34.280 AU
227.23 AU
Eccentricity 0.8491
3425.31 yr (1,251,096 days)
0° 0m 1.08s / day
Inclination 30.763°
Physical characteristics
Dimensions 222.59 km (derived)[4]
332±31 km[3][5]
336 km (radiometric)[6]
0.05 (radiometric)[6]
0.10 (assumed)[4]
IR [3][7] · C[4]
B–R = 1.38[3]
B–V = 0.860±0.040[8] · 0.820±0.048[9] · 0.820±0.020[7]
V–R = 0.520±0.040[8] · 0.572±0.038[9] · 0.580±0.020[7]
V–I = 1.070±0.060[8] · 1.013±0.072[9] · 1.060±0.010[7]
5.94±0.03 (R)[8] · 5.940±0.053 (R)[10] · 6.2[1] · 6.38[4][11] · 6.4[6]

(82158) 2001 FP185, provisional designation 2001 FP185, is a highly eccentric trans-Neptunian object from the scattered disc in the outermost part of the Solar System, approximately 330 kilometers in diameter. It was discovered on 26 March 2001, by American astronomer Marc Buie at Kitt Peak National Observatory in Arizona, United States.[2]

Orbit and classification[edit]

2001 FP185 is a scattered-disc object which belong to the most distant and coldest objects in the Solar System and are thought to be source of most periodic comets.

It orbits the Sun at a distance of 34.3–420.2 AU once every 3425 years and 4 months (1,251,096 days). Its orbit has an eccentricity of 0.85 and an inclination of 31° with respect to the ecliptic.[1] A first precovery was taken by the Sloan Digital Sky Survey in March 1999, extending the body's observation arc by 2 years prior to its official discovery observation at Kitt Peak.[2]

Planet Nine coorbital[edit]

If a massive trans-Neptunian object exists, like hypothetical Planet Nine, 2001 FP185 may be co-orbital with it.[12][13]

Physical characteristics[edit]

Spectra and colors[edit]

2001 FP185's color has extensively been measured.[7][8][9] The object has a determined BR and IR spectra, which are intermediate classes of the very blue BB and very red RR spectra.[3][7]

Diameter and albedo[edit]

According to astronomer Michael Brown and based on radiometric observations, 2001 FP185 measures 336 kilometers in diameter and its surface has an (assumed) albedo of 0.05.[6] Observations with the PACS-instrument of the Herschel Space Observatory during a survey of scattered-disc objects ("TNO are cool") found a similar diameter of 332 kilometer with an albedo of 0.046.[5] The Collaborative Asteroid Lightcurve Link assumes a higher albedo of 0.10 and consequently derives a much shorter diameter of 222 kilometers based on an absolute magnitude of 6.38.[4] Brown considers 2001 FP185 to be possibly a dwarf planet (see list).[6]


No rotational lightcurve of 2001 FP185 has been obtained from photometric observations. The body's rotation period, pole axis and brightness amplitude remains unknown.[4]

Numbering and naming[edit]

This minor planet was numbered by the Minor Planet Center on 4 May 2004.[14] As of 2018, it has not been named.[2]

See also[edit]


  1. ^ a b c d e "JPL Small-Body Database Browser: 82158 (2001 FP185)" (2015-06-22 last obs.). Jet Propulsion Laboratory. Retrieved 2 August 2017. 
  2. ^ a b c d e "82158 (2001 FP185)". Minor Planet Center. Retrieved 2 August 2017. 
  3. ^ a b c d e "List of Known Trans-Neptunian Objects". Johnston's Archive. 22 July 2017. Retrieved 2 August 2017. 
  4. ^ a b c d e f "LCDB Data for (82158)". Asteroid Lightcurve Database (LCDB). Retrieved 2 August 2017. 
  5. ^ a b c Santos-Sanz, P.; Lellouch, E.; Fornasier, S.; Kiss, C.; Pal, A.; Müller, T. G.; et al. (May 2012). ""TNOs are Cool": A survey of the trans-Neptunian region. IV. Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel-PACS" (PDF). Astronomy and Astrophysics. 541: 18. arXiv:1202.1481Freely accessible. Bibcode:2012A&A...541A..92S. doi:10.1051/0004-6361/201118541. Retrieved 2 August 2017. 
  6. ^ a b c d e "How many dwarf planets are there in the outer solar system?". Mike Brown. Retrieved 2 August 2017. 
  7. ^ a b c d e f 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 2 August 2017. 
  8. ^ a b c d e Jewitt, David; Peixinho, Nuno; Hsieh, Henry H. (November 2007). "U-Band Photometry of Kuiper Belt Objects". The Astronomical Journal. 134 (5): 2046–2053. Bibcode:2007AJ....134.2046J. doi:10.1086/522787. Retrieved 2 August 2017. 
  9. ^ a b c d Hainaut, O. R.; Boehnhardt, H.; Protopapa, S. (October 2012). "Colours of minor bodies in the outer solar system. II. A statistical analysis revisited" (PDF). Astronomy and Astrophysics. 546: 20. arXiv:1209.1896Freely accessible. Bibcode:2012A&A...546A.115H. doi:10.1051/0004-6361/201219566. Retrieved 2 August 2017. 
  10. ^ 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:1206.3153Freely accessible. Bibcode:2012A&A...546A..86P. doi:10.1051/0004-6361/201219057. Retrieved 2 August 2017. 
  11. ^ Romanishin, W.; Tegler, S. C. (December 2005). "Accurate absolute magnitudes for Kuiper belt objects and Centaurs". Icarus. 179 (2): 523–526. Bibcode:2005Icar..179..523R. doi:10.1016/j.icarus.2005.06.016. Retrieved 2 August 2017. 
  12. ^ de la Fuente Marcos, C.; de la Fuente Marcos, R. (September 2014). "Extreme trans-Neptunian objects and the Kozai mechanism: signalling the presence of trans-Plutonian planets" (PDF). Monthly Notices of the Royal Astronomical Society: Letters. 443 (1): L59–L63. arXiv:1406.0715Freely accessible. Bibcode:2014MNRAS.443L..59D. doi:10.1093/mnrasl/slu084. Retrieved 2 August 2017. 
  13. ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raú; l; Aarseth, Sverre J. (January 2015). "Flipping minor bodies: what comet 96P/Machholz 1 can tell us about the orbital evolution of extreme trans-Neptunian objects and the production of near-Earth objects on retrograde orbits" (PDF). Monthly Notices of the Royal Astronomical Society. 446 (2): 1867–1873. arXiv:1410.6307Freely accessible. Bibcode:2015MNRAS.446.1867D. doi:10.1093/mnras/stu2230. Retrieved 2 August 2017. 
  14. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018. 

External links[edit]