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10199 Chariklo

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"Chariklo" redirects here. For either of the Ancient Greek nymphs, see Chariclo.

10199 Chariklo /ˈkærəkloʊ/ is the largest confirmed centaur, a class of minor planet in the outer Solar System. It orbits the Sun between Saturn and Uranus, grazing the orbit of Uranus. On 26 March 2014, astronomers announced the discovery of two rings (nicknamed Oiapoque and Chuí after the rivers that define Brazil's borders)[22] around Chariklo by observing a stellar occultation,[23][24] making it the first minor planet known to have rings.[25][26]

10199 Chariklo
Hubble Space Telescope image of Chariklo taken in 2015
Discovery[1][2]
Discovered bySpacewatch (J. Scotti)
Discovery siteKitt Peak Obs.
Discovery date15 February 1997
Designations
(10199) Chariklo
Pronunciation/ˈkærəkloʊ/[3]
Named after
Χαρικλώ Khariklō
(Ancient Greek nymph)[4]
1997 CU26
centaur[1][5] · distant[2]
AdjectivesCharikloan, Charikloian /kærəˈkloʊ(i)ən/
Symbol
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 1
Observation arc26.51 yr (9,684 days)
Earliest precovery date5 November 1988
Aphelion18.545 AU
Perihelion13.099 AU
15.822 AU
Eccentricity0.1721
62.93 yr (22,987 days)
77.670°
0° 0m 56.52s / day
Inclination23.382°
300.42°
  • 25 June 2066[6]
  • 17 December 2003 (previous)
242.90°
Known satellites(2) rings of Chariklo · (undiscovered embedded or shepherd moons?)[7]
Jupiter MOID8.1850 AU
TJupiter3.4820
Physical characteristics
248±18 km[8]
254 km[7]
(296x264x204 km)[9]
(287.6x270.4x198.2 km)[10]
7.004±0.036 h[5]
0.045±0.010
0.10±0.02[11]
0.035±0.010[8]
0.042±0.005[5]
0.057 (assumed)[5]
SMASS = D[1] · D[5]
BR (G-mode)[12][13][14]
B−V = 0.84[14]
V−R = 0.50±0.03[14]
B−R = 1.34[14]
V−I = 1.02±0.02[14]
R−J = 0.99[14]
V−J = 1.49±0.07[14]
J−H = 0.49[14]
V−H = 1.98±0.08[14]
18.3[15]
6.569±0.015 (R)[16] · 6.6[1] · 6.65[5][17] · 6.75[18] · 6.76[19][20] · 7.07±0.04[12] · 7.08±0.04[21] · 7.03±0.10[5] · 7.40±0.25[8]

A photometric study in 2001 was unable to find a definite period of rotation.[27] Infrared observations of Chariklo indicate the presence of water ice,[28] which may in fact be located in its rings.[7]

Discovery and naming

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Chariklo was discovered by James V. Scotti of the Spacewatch program on February 15, 1997. Chariklo is named after the nymph Chariclo (Χαρικλώ), the wife of Chiron and the daughter of Apollo.[2][4]

A symbol derived from that for 2060 Chiron,  , was devised in the late 1990s by German astrologer Robert von Heeren. It replaces Chiron's K with a C for Chariklo.[29]

Size and shape

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Chariklo is currently the largest known centaur, with a volume-equivalent diameter of about 250 km.[10] Its shape is probably elongated, with dimensions of 287.6 × 270.4 × 198.2 km.[10] (523727) 2014 NW65 is likely to be the second largest with 225 km (140 mi) and 2060 Chiron is likely to be the third largest with 220 km (140 mi).[8]

Orbit

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Centaurs originated in the Kuiper belt and are in dynamically unstable orbits that will lead to ejection from the Solar System, an impact with a planet or the Sun, or transition into a short-period comet.[30]

The orbit of Chariklo is more stable than those of Nessus, Chiron, and Pholus. Chariklo lies within 0.09 AU of the 4:3 resonance of Uranus and is estimated to have a relatively long orbital half-life of about 10.3 Myr.[31] Orbital simulations of twenty clones of Chariklo suggest that Chariklo will not start to regularly come within 3 AU (450 Gm) of Uranus for about thirty thousand years.[32]

During the perihelic oppositions of 2003–04, Chariklo had an apparent magnitude of +17.7.[33] As of 2014, Chariklo was 14.8 AU from the Sun.[15]

 

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Rings

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Main article: Rings of Chariklo

A stellar occultation in 2013[7][22] revealed that Chariklo has two rings with radii 386 and 400 km and widths of about 6.9 km and 0.12 km respectively.[10] The rings are approximately 14 km apart.[10] This makes Chariklo the smallest known object to have rings. These rings are consistent with an edge-on orientation in 2008, which can explain Chariklo's dimming before 2008 and brightening since. Nonetheless, the elongated shape of Chariklo explains most of the brightness variability resulting in darker rings than previously determined.[9] Furthermore, the rings can explain the gradual disappearance of the water-ice features in Chariklo's spectrum before 2008 and their reappearance thereafter if the water ice is in Chariklo's rings.[7][23][34]

 
An infographic showing the apparent brightness measurement during Chariklo's occultation

The existence of a ring system around a minor planet was unexpected because it had been thought that rings could only be stable around much more massive bodies. Ring systems around minor bodies had not previously been discovered despite the search for them through direct imaging and stellar occultation techniques.[7] Chariklo's rings should disperse over a period of at most a few million years, so either they are very young, or they are actively contained by shepherd moons with a mass comparable to that of the rings.[35][7][23][34] However, other research suggests that Chariklo's elongated shape combined with its fast rotation can clear material in an equatorial disk through Lindblad resonances and explain the survival and location of the rings, a mechanism valid also for the ring of Haumea.[36]

The team nicknamed the rings Oiapoque (the inner, more substantial ring) and Chuí (the outer ring), after the two rivers that form the northern and southern coastal borders of Brazil. A request for formal names will be submitted to the IAU at a later date.[23]

It has been confirmed that 2060 Chiron may have a similar pair of rings.[37]

Exploration

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Main article: Camilla (spacecraft)

Camilla is a mission concept published in June 2018 that would launch a robotic probe to perform a single flyby of Chariklo and drop off a 100 kg (220 lb) impactor made of tungsten to excavate a crater approximately 10 m (33 ft) deep for remote compositional analysis during the flyby.[38] The mission would be designed to fit under the cost cap of NASA's New Frontiers program, although it has not been formally proposed to compete for funding. The spacecraft would be launched in September 2026, using one gravity assist from Venus in February 2027 and Earth in December 2027 and 2029 to accelerate it out toward Jupiter.

See also

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References

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  1. ^ a b c d e "JPL Small-Body Database Browser: 10199 Chariklo (1997 CU26)" (2015-05-12 last obs.). Jet Propulsion Laboratory. Retrieved 16 August 2017.
  2. ^ a b c "10199 Chariklo (1997 CU26)". Minor Planet Center. Retrieved 16 August 2017.
  3. ^ Noah Webster (1884) A Practical Dictionary of the English Language
  4. ^ a b Schmadel, Lutz D. (2007). "(10199) Chariklo". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 725. doi:10.1007/978-3-540-29925-7_7876. ISBN 978-3-540-00238-3.
  5. ^ a b c d e f g "LCDB Data for (10199) Chariklo". Asteroid Lightcurve Database (LCDB). Retrieved 16 August 2017.
  6. ^ "Horizons Batch for 10199 Chariklo (1997 CU26) on 2066-Jun-25" (Perihelion occurs when rdot flips from negative to positive). JPL Horizons. Retrieved 25 June 2022. (JPL#41 Soln.date: 2022-Jun-09)
  7. ^ a b c d e f g Braga-Ribas, F.; Sicardy, B.; Ortiz, J. L.; Snodgrass, C.; Roques, F.; Vieira-Martins, R.; et al. (April 2014). "A ring system detected around the Centaur (10199) Chariklo". Nature. 508 (7494): 72–75. arXiv:1409.7259. Bibcode:2014Natur.508...72B. doi:10.1038/nature13155. ISSN 0028-0836. PMID 24670644. S2CID 4467484.
  8. ^ a b c d Fornasier, S.; Lellouch, E.; Müller, T.; Santos-Sanz, P.; Panuzzo, P.; Kiss, C.; et al. (July 2013). "TNOs are Cool: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of nine bright targets at 70–500 μm". Astronomy and Astrophysics. 555: 22. arXiv:1305.0449. Bibcode:2013A&A...555A..15F. doi:10.1051/0004-6361/201321329. S2CID 119261700.
  9. ^ a b Leiva, R.; Sicardy, B.; Camargo, J.I.B (August 2017). "Size and shape of Chariklo from multi-epoch stellar occultations". The Astronomical Journal. 154 (4): 159. arXiv:1708.08934. Bibcode:2017AJ....154..159L. doi:10.3847/1538-3881/aa8956. S2CID 54032928.
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  15. ^ a b "AstDys (10199) Chariklo Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 10 February 2010.
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  26. ^ Sokol, J. (20 February 2017). "The upstart asteroid who showed rings are for everybody". New Scientist. Retrieved 22 February 2017.
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  28. ^ Jewitt; Brown (17 April 2001). "Infrared Observations of Centaur 10119 Chariklo with possible surface variation" (PDF). Archived from the original (PDF) on 29 November 2004. Retrieved 9 November 2006.
  29. ^ Miller, Kirk; Stein, Zane (26 August 2021). "Comment on U+26B7 CHIRON" (PDF). L2/21-225.
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  31. ^ Horner, J.; Evans, N.W.; Bailey, M. E. (2004). "Simulations of the Population of Centaurs I: The Bulk Statistics". Monthly Notices of the Royal Astronomical Society. 354 (3): 798–810. arXiv:astro-ph/0407400. Bibcode:2004MNRAS.354..798H. doi:10.1111/j.1365-2966.2004.08240.x. S2CID 16002759.
  32. ^ "Twenty clones of Centaur 10199 Chariklo making passes within 450Gm". Archived from the original on 25 October 2012. Retrieved 9 May 2009. (Solex 10) Archived 2008-12-20 at the Wayback Machine. Accessed 2009-05-10.
  33. ^ "AstDys (10199) Chariklo (March 2003) Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 3 April 2009.
  34. ^ a b Gibney, E. (26 March 2014). "Asteroids can have rings too". Nature. doi:10.1038/nature.2014.14937. S2CID 211729137.
  35. ^ Sickafoose, Amanda A.; Lewis, Mark C. (6 February 2024). "Numerical Simulations of (10199) Chariklo's Rings with a Resonant Perturber". The Planetary Science Journal. 5 (32): 32. doi:10.3847/PSJ/ad151c.
  36. ^ Sicardy, B.; Leiva, R.; Renner, S.; Roques, F.; El Moutamid, M.; Santos-Sanz, P.; Desmars, J. (19 November 2018). "Ring dynamics around non-axisymmetric bodies with application to Chariklo and Haumea". Nature Astronomy. 3 (2): 146–153. arXiv:1811.09437. doi:10.1038/s41550-018-0616-8. ISSN 2397-3366. S2CID 119236027.
  37. ^ Ortiz, J.L.; Duffard, R.; Pinilla-Alonso, N.; Alvarez-Candal, A.; Santos-Sanz, P.; Morales, N.; Fernández-Valenzuela, E.; Licandro, J.; Campo Bagatin, A.; Thirouin, A. (2015). "Possible ring material around centaur (2060) Chiron". Astronomy & Astrophysics. 576: A18. arXiv:1501.05911. Bibcode:2015A&A...576A..18O. doi:10.1051/0004-6361/201424461. S2CID 38950384.
  38. ^ Howell, Samuel M.; Chou, Luoth; Thompson, Michelle; Bouchard, Michael C.; Cusson, Sarah; Marcus, Matthew L.; Smith, Harrison B.; Bhattaru, Srinivasa; Blalock, John J.; Brueshaber, Shawn; Eggl, Siegfried; Jawin, Erica R.; Miller, Kelly; Rizzo, Maxime; Steakley, Kathryn; Thomas, Nancy H.; Trent, Kimberly R.; Ugelow, Melissa; Budney, Charles J.; Mitchell, Karl L.; Lowes, Leslie (2018). "Camilla: A centaur reconnaissance and impact mission concept" (PDF). Planetary and Space Science. 164: 184–193. Bibcode:2018P&SS..164..184H. doi:10.1016/j.pss.2018.07.008. S2CID 126013385.
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