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14832 Alechinsky, provisional designation 1987 QC3, is a Vestian asteroid from the inner regions of the asteroid belt, approximately 4 kilometers (2.5 miles) in diameter. It was discovered on 27 August 1987, by Belgian astronomer Eric Elst at ESO's La Silla Observatory site in northern Chile.[1] The highly elongated asteroid has a rotation period of 8.1 hours.[5] It was named after Belgian painter Pierre Alechinsky.[2]

14832 Alechinsky
Discovery [1]
Discovered byE. W. Elst
Discovery siteLa Silla Obs.
Discovery date27 August 1987
MPC designation(14832) Alechinsky
Named after
Pierre Alechinsky[1][2]
(Belgian painter)
1987 QC3 · 1994 PY32
main-belt[1][3] · (inner)
Orbital characteristics[3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc30.76 yr (11,234 d)
Aphelion2.5765 AU
Perihelion2.0088 AU
2.2926 AU
3.47 yr (1,268 d)
0° 17m 2.04s / day
Physical characteristics
Mean diameter
3.92 km (calculated)[5]
4.359±0.176 km[6][7]
8.07±0.02 h[8]
0.24 (assumed)[5]
S (assumed)[5]
14.462±0.010 (R)[9]

Orbit and classificationEdit

Alechinsky is a member of the Vesta family. Vestian asteroids have a composition akin to cumulate eucrites (HED meteorites) and are thought to have originated deep within 4 Vesta's crust, possibly from the Rheasilvia crater, a large impact crater on its southern hemisphere near the South pole, formed as a result of a subcatastrophic collision. It orbits the Sun in the inner main-belt at a distance of 2.0–2.6 AU once every 3 years and 6 months (1,268 days; semi-major axis of 2.29 AU). Its orbit has an eccentricity of 0.12 and an inclination of 6° with respect to the ecliptic.[3] The asteroid's observation arc begins in 1987, as no precoveries had been taken prior to its discovery.[1]


This minor planet was named in honor of Belgian painter and internationally prominent 20th century artist, Pierre Alechinsky (born 1927), known for his treatment of colors, versatility and graphic humor. He was a member of the expressionist art group and avant-garde movement CoBrA, a name which was coined from the initials of the members' home cities: Copenhagen, Brussels, and Amsterdam.[2] The approved naming citation was published by the Minor Planet Center on 13 October 2000 (M.P.C. 41387).[10]

Physical characteristicsEdit

Diameter and albedoEdit

According to the survey carried out by the NEOWISE mission of NASA's space-based Wide-field Infrared Survey Explorer, Alechinsky measures 4.4 kilometers in diameter and its surface has an albedo of 0.194,[6] while the Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – which derives from 8 Flora, the largest member and namesake of this orbital family – and calculates a diameter of 3.9 kilometers with an absolute magnitude of 14.2.[5]

Rotation periodEdit

In February 2013, two rotational lightcurves of Alechinsky were obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory, California. Lightcurve analysis gave a rotation period of 8.07±0.02 and 9.5831±0.1453 hours, with a brightness variation of 0.98 and 1.30 in magnitude, respectively (U=2+/2).[8][9] Such an exceptionally high amplitude in magnitude indicates that the body has a very elongated shape.


  1. ^ a b c d e f "14832 Alechinsky (1987 QC3)". Minor Planet Center. Retrieved 27 July 2018.
  2. ^ a b c Schmadel, Lutz D. (2007). "(14832) Alechinsky". Dictionary of Minor Planet Names – (14832) Alechinsky. Springer Berlin Heidelberg. p. 817. doi:10.1007/978-3-540-29925-7_9052. ISBN 978-3-540-00238-3.
  3. ^ a b c d "JPL Small-Body Database Browser: 14832 Alechinsky (1987 QC3)" (2018-05-25 last obs.). Jet Propulsion Laboratory. Retrieved 27 July 2018.
  4. ^ "Asteroid 14832 Alechinsky". Small Bodies Data Ferret. Retrieved 27 July 2018.
  5. ^ a b c d e f "LCDB Data for (14832) Alechinsky". Asteroid Lightcurve Database (LCDB). Retrieved 6 April 2016.
  6. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 8 May 2016.
  7. ^ a b Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. Retrieved 3 December 2016.
  8. ^ a b Chang, Chan-Kao; Ip, Wing-Huen; Lin, Hsing-Wen; Cheng, Yu-Chi; Ngeow, Chow-Choong; Yang, Ting-Chang; et al. (June 2014). "313 New Asteroid Rotation Periods from Palomar Transient Factory Observations". The Astrophysical Journal. 788 (1): 21. arXiv:1405.1144. Bibcode:2014ApJ...788...17C. doi:10.1088/0004-637X/788/1/17. Retrieved 6 April 2016.
  9. ^ a b Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 6 April 2016.
  10. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 27 July 2018.

External linksEdit