65 Cybele

65 Cybele
Discovery [1][2]
Discovered byE. W. Tempel
Discovery siteMarseille Obs.
Discovery date8 March 1861
Designations
(65) Cybele
Pronunciation/ˈsɪbəliː/[3]
Named after
Cybele [4]
(Hellenistic deity)
1949 YQ
main belt · (outer)[1]
Cybele[5]
AdjectivesCybelean /ˌsɪbəˈliːən/, rarely Cybelian /sɪˈbɛliən/
Orbital characteristics
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc155.98 yr (56,971 d)
Aphelion3.8102 AU
Perihelion3.0464 AU
3.4283 AU
Eccentricity0.1114
6.35 yr (2,319 days)
168.06°
0° 9m 19.08s / day
Inclination3.5627°
155.63°
102.37°
Physical characteristics
Dimensions297 km × 291 km × 213 km[6]
263±3 km[6]
Massest. (14.8±1.8)×1018 kg[6]
Mean density
1.55±0.19 g/cm3[6]
3.98704 h[7]
4.036 h[8]
4.04 h[9]
4.04052 h[10][11]
6.07 h[12]
6.07 h[13]
6.08±0.05 h[14]
6.081±0.001 h[a]
6.0814±0.0001 h[15]
6.081434±0.000005 h[16]
6.082±0.001 h[17]
0.044[18]
0.050±0.005[19]
0.06±0.03[20]
0.06±0.04[21]
0.0706±0.003[22][23]
Tholen = P [1]
SMASS = Xc [1] · X [23]
B–V = 0.690[1]
U–B = 0.271[1]
V–R = 0.400±0.007[24]
10.67 to 13.64
6.58±0.06[24] · 6.62[1][22][23][21][18] · 6.88±0.26[25] · 6.95[20]

65 Cybele is one of the largest asteroids in the Solar System. It is located in the outer asteroid belt. It is thought to be a remnant primordial body.[6] It gives its name to the Cybele group of asteroids[5] that orbit outward from the Sun from the 2:1 orbital resonance with Jupiter. The X-type asteroid has a relatively short rotation period of 6.0814 hours. It was discovered by Wilhelm Tempel in 1861, and named after Cybele, the earth goddess.

Discovery and naming

Cybele was discovered on 8 March 1861, by German astronomer Wilhelm Tempel from the Marseilles Observatory in southeastern France.[2] A minor controversy arose from its naming process. Tempel had awarded the honour of naming the asteroid to Carl August von Steinheil in recognition of his achievements in telescope production. Von Steinheil elected to name it "Maximiliana" after the reigning monarch Maximilian II of Bavaria. At the time, asteroids were conventionally given classical names, and a number of astronomers protested this contemporary appellation. The name Cybele was chosen instead, referring to the Phrygian goddess of the earth.[4] (The previously discovered 45 Eugenia, 54 Alexandra, and 64 Angelina had nevertheless also been given non-classical names; 64 Angelina had also been discovered by Tempel, but its name stood despite similar protests.)

Physical characteristics

The first Cybelian stellar occultation was observed on 17 October 1979, in the Soviet Union. The asteroid appeared to have an irregular shape, with the longest chord being measured as 245 km, closely matching results determined by the IRAS satellite in 1983 (see below). During the same 1979 occultation, a hint of a possible 11 km wide minor-planet moon at 917 km distance was detected,[26] but has since never been corroborated. As of 2017, neither the Asteroid Lightcurve Data Base nor Johnston's archive consider Cybele to be a binary asteroid.[23][27]

Diameter estimates

Mean diameter estimates for Cybele range between 218.56 and 300.54 kilometers. According to observations by the Infrared Astronomical Satellite IRAS in 1983, the asteroid has a diameter of 237.26 km.[22] The NEOWISE mission of NASA's Wide-field Infrared Survey Explorer gave a diameter of 218.56 and 276.58 km.[20][21] The largest estimates of 300.54 km is from the Japanese Akari satellite.[18] In 2004, Müller estimated Cybele using thermophysical modelling (TPM) to have dimensions of 302 × 290 × 232 km, which corresponds to a mean-diameter of 273.0 km.[19]

Observations in 2021 show that Cybele's present shape very closely matches what would be expected if it were in hydrostatic equilibrium, in contrast to the other large Cybele asteroids 87 Sylvia and 107 Camilla. This suggests a transition point between irregular small asteroids and equilibrium larger bodies at around 1.5 × 1019 kg, and makes it possible that outer Solar System bodies at least 260 km in diameter might have formed in equilibrium (note Saturn IX Phoebe, which at 212 km diameter probably formed in equilibrium). However, it is not certain if Cybele's current shape is its primordial one, or if it is the result of a large impact as on the very round 10 Hygiea and 31 Euphrosyne. Today no Cybele family is observable, but since Cybele orbits in a rather unstable region, any such family would be dispersed within 2 billion years. Cybele's larger density compared to Sylvia and Camilla does somewhat favour the first hypothesis, though. (Sylvia and Camilla experienced impacts, as evidenced by their satellites and by the Sylvia family.)[28]

Spectrum

Examination of the asteroid's infrared spectrum shows an absorption feature that is similar to the one present in the spectrum of 24 Themis. This can be explained by the presence of water ice. The asteroid may be covered in a layer of fine silicate dust mixed with small amounts of water-ice and organic solids.[29]

Recent occultations

On August 24, 2008, Cybele occulted 2UCAC 24389317, a 12.7-magnitude star in the constellation Ophiuchus which showed a long axis of at least 294 km.[30] On 11 October 2009, Cybele occulted a 13.4-magnitude star in the constellation Aquarius.[31]

Notes

  1. ^ Pilcher (2014m). Rotation period for (65) Cybele: 6.081±0.001 hours with a brightness amplitude of 0.03±0.01 mag. Quality Code of 3−. Summary figures at the LCDB; not available as 2014MPBu...41..250F at ADS

References

  1. ^ a b c d e f g "JPL Small-Body Database Browser: 65 Cybele" (2017-11-26 last obs.). Jet Propulsion Laboratory. Retrieved 22 December 2017.
  2. ^ a b "(65) Cybele". Minor Planet Center. Retrieved 21 April 2017.
  3. ^ Noah Webster (1884) A Practical Dictionary of the English Language
  4. ^ a b Schmadel, Lutz D. (2007). "(65) Cybele". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 21. doi:10.1007/978-3-540-29925-7_66. ISBN 978-3-540-00238-3.
  5. ^ a b Linda T. Elkins-Tanton – Asteroids, Meteorites, and Comets (2010) – Page 96 (Google Books)
  6. ^ a b c d e Marsset et al. (2022) The equilibrium shape of (65) Cybele: primordial or relic of a large impact?
  7. ^ Drummond, J. D.; Weidenschilling, S. J.; Chapman, C. R.; Davis, D. R. (October 1988). "Photometric geodesy of main-belt asteroids. II – Analysis of lightcurves for poles, periods, and shapes". Icarus. 76 (1): 19–77. Bibcode:1988Icar...76...19D. doi:10.1016/0019-1035(88)90139-X. ISSN 0019-1035. Retrieved 22 December 2017.
  8. ^ Shevchenko, V. G.; Chiorny, V. G.; Kalashnikov, A. V.; Krugly, Yu. N.; Mohamed, R. A.; Velichko, F. P. (February 1996). "Magnitude-phase dependences for three asteroids". Astronomy and Astrophysics Supplement. 115: 475–479. Bibcode:1996A&AS..115..475S. Retrieved 22 December 2017.
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  10. ^ De Angelis, G. (May 1995). "Asteroid spin, pole and shape determinations". Planetary and Space Science. 43 (5): 649–682. Bibcode:1995P&SS...43..649D. doi:10.1016/0032-0633(94)00151-G. Retrieved 22 December 2017.
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  15. ^ Pilcher, Frederick (April 2012). "Rotation Period Determinations for 31 Euphrosyne, 65 Cybele, 154 Bertha 177 Irma, 200 Dynamene, 724 Hapag, 880 Herba, and 1470 Carla". The Minor Planet Bulletin. 39 (2): 57–60. Bibcode:2012MPBu...39...57P. ISSN 1052-8091. Retrieved 22 December 2017.
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  17. ^ Pilcher, Frederick (January 2010). "Rotation Period Determination for 65 Cybele". The Minor Planet Bulletin. 37 (1): 8. Bibcode:2010MPBu...37....8P. ISSN 1052-8091. Retrieved 22 December 2017.
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  19. ^ a b Müller, T. G.; Blommaert, J. A. D. L. (April 2004). "65 Cybele in the thermal infrared: Multiple observations and thermophysical analysis". Astronomy and Astrophysics. 418: 347–356. arXiv:astro-ph/0401458. Bibcode:2004A&A...418..347M. doi:10.1051/0004-6361:20040025. S2CID 18524619. Retrieved 21 April 2017.
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  24. ^ a b Warner, Brian D. (December 2007). "Initial Results of a Dedicated H-G Project". The Minor Planet Bulletin. 34 (4): 113–119. Bibcode:2007MPBu...34..113W. ISSN 1052-8091. Retrieved 22 December 2017.
  25. ^ 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. S2CID 53493339. Retrieved 19 October 2017.
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  28. ^ Marsset, M.; Brož, M.; Vermersch, J.; Rambaux, N.; Ferrais, M.; Viikinkoski, M.; Hanuš, J.; Jehin, E.; Podlewska-Gaca, E.; Bartczak, P.; Dudziński, G.; Carry, B.; Vernazza, P.; Szakáts, R.; Duffard, R.; Jones, A.; Molina, D.; Santana-Ros, T.; Benkhaldoun, Z.; Birlan, M.; Dumas, C.; Fétick, R.; Fusco, T.; Jorda, L.; Marchis, F.; Vachier, F.; Yang, B. (2023). "The equilibrium shape of (65) Cybele: Primordial or relic of a large impact?". Astronomy & Astrophysics. 670: A52. arXiv:2212.00680. Bibcode:2023A&A...670A..52M. doi:10.1051/0004-6361/202243859.
  29. ^ Licandro, J.; Campins, H.; Kelley, M.; Hargrove, K.; Pinilla-Alonso, N.; Cruikshank, D.; et al. (January 2011). "(65) Cybele: detection of small silicate grains, water-ice, and organics". Astronomy and Astrophysics. 525: 7. Bibcode:2011A&A...525A..34L. doi:10.1051/0004-6361/201015339.
  30. ^ IOTA. "(65) Cybele 2008 Aug 24 profile". Archived from the original on 3 March 2012. Retrieved 2 December 2010.
  31. ^ Steve Preston. "(65) Cybele / 2UCAC 28838190 event on 2009 Oct 11, 01:30 UT". Retrieved 21 September 2009.[permanent dead link]