9916 Kibirev
Get 9916 Kibirev essential facts below. View Videos or join the 9916 Kibirev discussion. Add 9916 Kibirev to your PopFlock.com topic list for future reference or share this resource on social media.
9916 Kibirev
9916 Kibirev
Discovery [1]
Discovered byN. Chernykh
Discovery site
Discovery date3 October 1978
MPC designation(9916) Kibirev
Named after
Sergej Kibirev[1]
(Russian informatician)
main-belt[1][2] · (outer)
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc44.52 yr (16,261 d)
Aphelion3.0950 AU
Perihelion2.6050 AU
2.8500 AU
4.81 yr (1,757 d)
0° 12m 17.28s / day
Physical characteristics
Mean diameter
S (assumed)[4]

9916 Kibirev, provisional designation , is a Koronian asteroid from the outer regions of the asteroid belt, approximately 6 kilometers (3.7 miles) in diameter. It was discovered on 3 October 1978, by astronomer Nikolai Chernykh at the Crimean Astrophysical Observatory in Nauchnij, on the Crimean peninsula. The likely S-type asteroid has a rotation period of about 15.2 hours and was named after Russian informatician Sergej Kibirev.[1][4]

Orbit and classification

Orbit of Kibirev (blue) with the inner planets and Jupiter in red

Kibirev is a core member of the Koronis family (605),[4][3] a very large outer asteroid family with nearly co-planar ecliptical orbits.[10] It orbits the Sun in the outer main-belt at a distance of 2.6-3.1 AU once every 4 years and 10 months (1,757 days; semi-major axis of 2.85 AU). Its orbit has an eccentricity of 0.09 and an inclination of 1° with respect to the ecliptic.[2] The body's observation arc begins with a precovery taken at Palomar Observatory in September 1973, or 5 years prior to its official discovery observation.[1]

Physical characteristics

Kibirev is an assumed S-type asteroid,[4] which is also the Koronis family's overall spectral type.[10]:23

Rotation period

In 2014, two rotational lightcurves of Kibirev were obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California.[7][8] Lightcurve analysis gave a rotation period of 15.171 and 15.48 hours with a brightness amplitude of 0.36 and 0.45 magnitude, respectively (U=2/2).[4]

Diameter and albedo

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Kibirev measures 6.201 kilometers in diameter and its surface has an albedo between 0.260 and 0.2898.[5][6]

The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 and calculates a diameter of 5.49 kilometers based on an absolute magnitude of 13.47.[4]


This minor planet was named after Russian Sergej Feodosievich Kibirev (born 1950), who works on new methods to process information and organizes the production of microelectronics in the Russian city of Novosibirsk.[1] The official naming citation was published by the Minor Planet Center on 9 March 2001 (M.P.C. 42359).[11]


  1. ^ a b c d e f "9916 Kibirev (1978 TR2)". Minor Planet Center. Retrieved 2018.
  2. ^ a b c d "JPL Small-Body Database Browser: 9916 Kibirev (1978 TR2)" (2018-03-28 last obs.). Jet Propulsion Laboratory. Retrieved 2018.
  3. ^ a b "Asteroid 9916 Kibirev - Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 2019.
  4. ^ a b c d e f g h i j "LCDB Data for (9916) Kibirev". Asteroid Lightcurve Database (LCDB). Retrieved 2018.
  5. ^ a b c 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.
  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. (catalog)
  7. ^ a b c 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.
  8. ^ a b c Chang, Chan-Kao; Ip, Wing-Huen; Lin, Hsing-Wen; Cheng, Yu-Chi; Ngeow, Chow-Choong; Yang, Ting-Chang; et al. (August 2015). "Asteroid Spin-rate Study Using the Intermediate Palomar Transient Factory". The Astrophysical Journal Supplement Series. 219 (2): 19. arXiv:1506.08493. Bibcode:2015ApJS..219...27C. doi:10.1088/0067-0049/219/2/27.
  9. ^ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34-47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007.
  10. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). Identification and Dynamical Properties of Asteroid Families. Asteroids IV. pp. 297-321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
  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.



Music Scenes