10370 Hylonome

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10370 Hylonome
Discovery [1]
Discovered by D. C. Jewitt
J. X. Luu
Discovery site Mauna Kea Obs.
Discovery date 27 February 1995
Designations
MPC designation (10370) Hylonome
Named after
Hylonome
(Greek mythology)[2]
1995 DW2
distant[3] · centaur[4]
Neptune-crosser
Uranus-grazer
Orbital characteristics[1][5]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 3
Observation arc 15.27 yr (5,576 days)
Aphelion 31.367 AU
Perihelion 18.888 AU
25.127 AU
Eccentricity 0.2483
125.96 yr (46,007 days)
61.910°
0° 0m 28.08s / day
Inclination 4.1443°
178.07°
6.7926°
Jupiter MOID 13.4352 AU
Jupiter Tisserand parameter 4.4530
Physical characteristics
Dimensions 70±20 km[6]
74±16 km[7]
75.09 km (derived)[4]
0.051±0.030[7]
0.057 (assumed)[4]
C[4] · BR (color group)[8]
8.6[1] · 9.08±0.04 (R)[9] · 9.250±0.131 (R)[10] · 9.35[4][11] · 9.51±0.08[7] · 9.53[12][13]

10370 Hylonome (/hˈlɒnəm/; from Greek: ‘Υλονομη), provisional designation 1995 DW2, is a minor planet orbiting in the outer Solar System. The dark and icy body belongs to the class of centaurs and measures approximately 75 kilometers in diameter.

It was discovered on 27 February 1995, by English astronomer David C. Jewitt and Vietnamese American astronomer Jane Luu at the U.S. Mauna Kea Observatory in Hawaii, and later named after the mythological creature Hylonome.[2][3]

Classification and orbit[edit]

Centaurs are a large population of icy bodies in transition between trans-Neptunian objects (TNOs) and Jupiter-family comets (JFCs), their orbits being unstable due to perturbations by the giant planets.[7] Currently, Uranus controls Hylonome's perihelion and Neptune its aphelion.[14]

Hylonome is a carbonaceous C-type body that orbits the Sun at a distance of 18.9–31.4 AU once every 125 years and 12 months (46,007 days). Its orbit has an eccentricity of 0.25 and an inclination of 4° with respect to the ecliptic.[1] It is a Neptune-crosser, and an outer-grazer of the orbit of Uranus, which it hence does not cross. Its minimum orbital intersection distance with Neptune and Uranus is 0.35854 and 0.52875 AU, respectively.[3]

It is estimated to have a relatively long orbital half-life of about 6.37 million years.[14] In the year 3478, it will pass within approximately 85 gigameters of Uranus and its semi-major axis will be reduced from 25.1 to 23.5 AU.[15]

Physical characteristics[edit]

Observations with the infrared Spitzer Space Telescope indicate a diameter of 70±20 kilometers,[6] whereas the Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous bodies of 0.057, giving it a diameter of 75.1 kilometers, based on an absolute magnitude of 9.35.[4]

A study in 2014, using data from Spitzer's Multiband Imaging Photometer (MIPS) and Herschel's Photodetector Array Camera and Spectrometer, gave a low albedo 0.051±0.030 and a diameter of 74±16 kilometers, based on an absolute magnitude of 9.51±0.08. The study concluded that among the observed population of centaurs, there is no correlation between their sizes, albedos, and orbital parameters. However, the smaller the centaur, the more reddish it is.[7]

Naming[edit]

This minor planet was named for Hylonome, a female centaur in Greek mythology. In the epic tragedy, she lost her very much beloved husband, the handsome centaur Cyllarus, who was accidentally killed by a spear. Heartbroken, she then took her own life to join him by throwing herself on the spear.[2] The official naming citation was published on 26 July 2000 (M.P.C. 41030).[16]

References[edit]

  1. ^ a b c d "JPL Small-Body Database Browser: 10370 Hylonome (1995 DW2)" (2010-06-14 last obs.). Jet Propulsion Laboratory. Retrieved 4 December 2016. 
  2. ^ a b c Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (10370) Hylonome. Springer Berlin Heidelberg. p. 731. ISBN 978-3-540-00238-3. Retrieved 26 May 2016. 
  3. ^ a b c "10370 Hylonome (1995 DW2)". Minor Planet Center. Retrieved 26 May 2016. 
  4. ^ a b c d e f "LCDB Data for (10370) Hylonome". Asteroid Lightcurve Database (LCDB). Retrieved 26 May 2016. 
  5. ^ "(10370) Hylonome". AstDyS. University of Pisa. Retrieved 20 December 2008. 
  6. ^ a b John Stansberry; Will Grundy; Mike Brown; Dale Cruikshank; John Spencer; David Trilling; et al. (2007-02-20). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". arXiv:astro-ph/0702538Freely accessible [astro-ph]. 
  7. ^ a b c d e Duffard, R.; Pinilla-Alonso, N.; Santos-Sanz, P.; Vilenius, E.; Ortiz, J. L.; Mueller, T.; et al. (April 2014). ""TNOs are Cool": A survey of the trans-Neptunian region. XI. A Herschel-PACS view of 16 Centaurs". Astronomy and Astrophysics. 564: 17. arXiv:1309.0946Freely accessible. Bibcode:2014A&A...564A..92D. doi:10.1051/0004-6361/201322377. 
  8. ^ Belskaya, Irina N.; Barucci, Maria A.; Fulchignoni, Marcello; Dovgopol, Anatolij N. (April 2015). "Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo". Icarus. 250: 482–491. Bibcode:2015Icar..250..482B. doi:10.1016/j.icarus.2014.12.004. Retrieved 26 May 2016. 
  9. ^ Bauer, James M.; Meech, Karen J.; Fernández, Yanga R.; Pittichova, Jana; Hainaut, Olivier R.; Boehnhardt, Hermann; et al. (November 2003). "Physical survey of 24 Centaurs with visible photometry". Icarus. 166 (1): 195–211. Bibcode:2003Icar..166..195B. doi:10.1016/j.icarus.2003.07.004. 
  10. ^ Peixinho, N.; Delsanti, A.; Guilbert-Lepoutre, A.; Gafeira, R.; Lacerda, P. (October 2012). "The bimodal colors of Centaurs and small Kuiper belt objects" (PDF). Astronomy and Astrophysics. 546: 12. arXiv:1206.3153Freely accessible. Bibcode:2012A&A...546A..86P. doi:10.1051/0004-6361/201219057. Retrieved 26 May 2016. 
  11. ^ Davies, John K.; McBride, Neil; Ellison, Sara L.; Green, Simon F.; Ballantyne, David R. (August 1998). "Visible and Infrared Photometry of Six Centaurs". Icarus. 134 (2): 213–227. Bibcode:1998Icar..134..213D. doi:10.1006/icar.1998.5931. 
  12. ^ Romanishin, W.; Tegler, S. C. (March 1999). "Rotation rates of Kuiper-belt objects from their light curves". Nature. 398 (6723): 129–132. Bibcode:1999Natur.398..129R. doi:10.1038/18168. 
  13. ^ Romanishin, W.; Tegler, S. C. (December 2005). "Accurate absolute magnitudes for Kuiper belt objects and Centaurs". Icarus. 179 (2): 523–526. Bibcode:2005Icar..179..523R. doi:10.1016/j.icarus.2005.06.016. 
  14. ^ a b Horner, J.; Evans, N. W.; Bailey, M. E. (November 2004). "Simulations of the population of Centaurs - I. The bulk statistics" (PDF). Monthly Notices of the Royal Astronomical Society. 354 (3): 798–810. arXiv:astro-ph/0407400Freely accessible. Bibcode:2004MNRAS.354..798H. doi:10.1111/j.1365-2966.2004.08240.x. Retrieved 5 August 2016. 
  15. ^ "Fifty clones of Centaur 10370 Hylonome all passing within ~85Gm of Uranus in 3478 Oct". Archived from the original on 2009-04-29. Retrieved 2009-04-25.  (Solex 10) Archived 2009-04-29 on WebCite
  16. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 26 May 2016. 

External links[edit]