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1865 Cerberus

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For the moon of Pluto, see Kerberos (moon).

1865 Cerberus
Lightcurve-based 3D-model of Cerberus
Discovery[1]
Discovered byL. Kohoutek
Discovery siteBergedorf Obs.
Discovery date26 October 1971
Designations
(1865) Cerberus
Pronunciation/ˈsɜːrbərəs/
Named after
Cerberus (Greek mythology)[2]
1971 UA
NEO · Apollo[1][3]
AdjectivesCerberean, -ian /sɜːrˈbɪəriən/[4][5]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc45.05 yr (16,456 days)
Aphelion1.5844 AU
Perihelion0.5757 AU
1.0801 AU
Eccentricity0.4669
1.12 yr (410 days)
205.19°
0° 52m 41.16s / day
Inclination16.095°
212.93°
325.26°
Earth MOID0.1567 AU · 61 LD
Physical characteristics
Dimensions1.2 km (Gehrels)[1]
1.608 km[6]
1.61 km (taken)[7]
1.611±0.013 km[8]
6.800±0.006 h[9]
6.80328±0.00001 h[10]
6.803286±0.000005 h[11]
6.8039 h[12]
6.804±0.003 h[13]
6.81 h[14]
6.810±0.003 h[15]
6.87 h[16]
0.1118[6]
0.136±0.021[8]
0.22
0.50±0.29[17]
S (Tholen)[1] · S (SMASS)[1]
S[7][18]
B–V = 0.790[1]
U–B = 0.442[1]
16.45±0.07 (R)[12]
16.84[1][8]
16.965±0.04[6][7]
16.97±0.04[9]
16.97±0.13[15]

1865 Cerberus is a stony asteroid and near-Earth object of the Apollo group, approximately 1.6 kilometers in diameter. It was discovered on 26 October 1971, by Czech astronomer Luboš Kohoutek at the Hamburger Bergedorf Observatory, Germany, and given the provisional designation 1971 UA. It was named for Cerberus from Greek mythology.[2][3]

Orbit and classification

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Cerberus orbits the Sun at a distance of 0.6–1.6 AU once every 1 years and 1 month (410 days). Its orbit has an eccentricity of 0.47 and an inclination of 16° with respect to the ecliptic.[1]

The Apollo asteroid has an Earth minimum orbital intersection distance of 0.1567 AU (23,400,000 km), which corresponds to 61 lunar distances. It passes within 30 gigametres (Gm) of the Earth 7 times from the year 1900 to the year 2100, each time at a distance of 24.4 Gm to 25.7 Gm. It also makes close approaches to Mars and Venus.[1]

Physical characteristics

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In the Tholen and SMASS taxonomy, Cerberus is a common stony S-type asteroid,[1] composed of 65% plagioclase and 35% pyroxene.[19] It has a rotation period of 6.804 hours and a geometric albedo of 0.220.[1][7] With a maximum lightcurve range of 2.3,[12] Cerberus may be cigar shaped like 1I/ʻOumuamua.

Naming

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This minor planet is named after the figure from Greek mythology, Cerberus, a three-headed dog that guarded the entrance to Hades, the Underworld. His capture marked the last of the twelve labors of Hercules. It is also the name of an extinct constellation, Cerberus, now contained in the eastern part of Hercules.[2] (It should not be confused with Kerberos, a moon of the dwarf planet Pluto.) The official naming citation was published by the Minor Planet Center on 20 December 1974 (M.P.C. 3758).[20]

References

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  1. ^ a b c d e f g h i j k l m "JPL Small-Body Database Browser: 1865 Cerberus (1971 UA)" (2016-11-14 last obs.). Jet Propulsion Laboratory. Retrieved 9 June 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1865) Cerberus". Dictionary of Minor Planet Names – (1865) Cerberus. Springer Berlin Heidelberg. pp. 149–150. doi:10.1007/978-3-540-29925-7_1866. ISBN 978-3-540-00238-3.
  3. ^ a b "1865 Cerberus (1971 UA)". Minor Planet Center. Retrieved 12 December 2016.
  4. ^ R.W. Chapman (1939) Adjectives from Proper Names, Clarendon Press, Oxford, p. 56
  5. ^ "Cerberean". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  6. ^ a b c Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. Retrieved 12 December 2016.
  7. ^ a b c d "LCDB Data for (1865) Cerberus". Asteroid Lightcurve Database (LCDB). Retrieved 12 December 2016.
  8. ^ a b c 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.
  9. ^ a b Harris, A. W.; Young, J. W. (October 1989). "Asteroid lightcurve observations from 1979-1981". Icarus. 81 (2): 314–364. Bibcode:1989Icar...81..314H. doi:10.1016/0019-1035(89)90056-0. ISSN 0019-1035. Retrieved 12 December 2016.
  10. ^ Durech, J.; Vokrouhlický, D.; Baransky, A. R.; Breiter, S.; Burkhonov, O. A.; Cooney, W.; et al. (November 2012). "Analysis of the rotation period of asteroids (1865) Cerberus, (2100) Ra-Shalom, and (3103) Eger - search for the YORP effect". Astronomy and Astrophysics. 547: 9. arXiv:1210.2219. Bibcode:2012A&A...547A..10D. doi:10.1051/0004-6361/201219396. Retrieved 12 December 2016.
  11. ^ Hanus, J.; Delbo', M.; Durech, J.; Alí-Lagoa, V. (August 2015). "Thermophysical modeling of asteroids from WISE thermal infrared data - Significance of the shape model and the pole orientation uncertainties". Icarus. 256: 101–116. arXiv:1504.04199. Bibcode:2015Icar..256..101H. doi:10.1016/j.icarus.2015.04.014. Retrieved 12 December 2016.
  12. ^ a b c Detail: "Pravec2008web" at LCDB Data for (1865) Cerberus
  13. ^ Skiff, Brian A.; Bowell, Edward; Koehn, Bruce W.; Sanborn, Jason J.; McLelland, Kyle P.; Warner, Brian D. (July 2012). "Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS) - 2008 May through 2008 December". The Minor Planet Bulletin. 39 (3): 111–130. Bibcode:2012MPBu...39..111S. ISSN 1052-8091. Retrieved 12 December 2016.
  14. ^ Detail: "Pravec1999web" at LCDB Data for (1865) Cerberus
  15. ^ a b Wisniewski, W. Z.; Michalowski, T. M.; Harris, A. W.; McMillan, R. S. (March 1995). "Photoelectric Observations of 125 Asteroids". Abstracts of the Lunar and Planetary Science Conference. 26: 1511. Bibcode:1995LPI....26.1511W. Retrieved 12 December 2016.
  16. ^ Sárneczky, K.; Szabó, Gy.; Kiss, L. L. (June 1999). "CCD observations of 11 faint asteroids". Astronomy and Astrophysics Supplement. 137 (2): 363–368. Bibcode:1999A&AS..137..363S. doi:10.1051/aas:1999251. Retrieved 12 December 2016.
  17. ^ Thomas, C. A.; Trilling, D. E.; Emery, J. P.; Mueller, M.; Hora, J. L.; Benner, L. A. M.; et al. (September 2011). "ExploreNEOs. V. Average Albedo by Taxonomic Complex in the Near-Earth Asteroid Population". The Astronomical Journal. 142 (3): 12. Bibcode:2011AJ....142...85T. doi:10.1088/0004-6256/142/3/85. Retrieved 12 December 2016.
  18. ^ Thomas, Cristina A.; Emery, Joshua P.; Trilling, David E.; Delbó, Marco; Hora, Joseph L.; Mueller, Michael (January 2014). "Physical characterization of Warm Spitzer-observed near-Earth objects". Icarus. 228: 217–246. arXiv:1310.2000. Bibcode:2014Icar..228..217T. doi:10.1016/j.icarus.2013.10.004. Retrieved 12 December 2016.
  19. ^ L.A. Lebofsky; M.L. Nelson. "Compositions of Near-Earth Asteroids" (PDF). University of Arizona. Retrieved 6 November 2015.
  20. ^ Schmadel, Lutz D. (2009). "Appendix – Publication Dates of the MPCs". Dictionary of Minor Planet Names – Addendum to Fifth Edition (2006–2008). Springer Berlin Heidelberg. p. 221. doi:10.1007/978-3-642-01965-4. ISBN 978-3-642-01964-7.
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