10370 Hylonome
Hubble Space Telescope image of Hylonome taken in 2009
Discovery[1]
Discovered byD. C. Jewitt
J. X. Luu
Discovery siteMauna Kea Obs.
Discovery date27 February 1995
Designations
(10370) Hylonome
Pronunciation/haɪˈlɒnəmiː/[2]
Named after
Ὑλονόμη Hylonomē
(Greek mythology)[3]
1995 DW2
centaur[4] · distant[1]
Neptune-crosser
Uranus-grazer
Symbol (astrological)
Orbital characteristics[4]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 3
Observation arc15.27 yr (5,576 days)
Aphelion31.393 AU
Perihelion18.910 AU
25.152 AU
Eccentricity0.2482
126.14 yr (46,073 days)
63.271°
0° 0m 28.08s / day
Inclination4.1443°
178.08°
7.0279°
Jupiter MOID13.4570 AU
TJupiter4.4550
Physical characteristics
Mean diameter
70±20 km[5]
74±16 km[6]
0.051±0.030[6]
BR (intermed. blue-red)[7][8]
8.6[4] · 9.08±0.04 (R)[9] · 9.250±0.131 (R)[10] · 9.35[7][11] · 9.51±0.08[6] · 9.53[12][13]

    10370 Hylonome (/haɪˈlɒnəmiː/; prov. 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 72 kilometers (45 miles) 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.[3][1]

    Classification and orbit

    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.[6] Currently, Uranus controls Hylonome's perihelion and Neptune its aphelion.[14]

    Hylonome is a carbonaceous C-type body that orbits the Sun in the outer main-belt at a distance of 18.9–31.4 AU once every 126 years and 2 months (46,073 days). Its orbit has an eccentricity of 0.25 and an inclination of 4° with respect to the ecliptic.[4] 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.[1]

    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]

    Naming

    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.[3] The official naming citation was published on 26 July 2000 (M.P.C. 41030).[16]

    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 Greek capital upsilon (Υ) for Hylonome (Ὑλονόμη).[17]

    Physical characteristics

    Observations with the infrared Spitzer Space Telescope indicate a diameter of 70±20 kilometers,[5] whereas the Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous bodies of 0.057, giving it a diameter of 75.1 kilometers with an absolute magnitude of 9.35.[7][18]

    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.[6]

    See also

    References

    1. 1 2 3 4 "10370 Hylonome (1995 DW2)". Minor Planet Center. Retrieved 26 May 2016.
    2. ↑ Noah Webster (1884) A Practical Dictionary of the English Language
    3. 1 2 3 Schmadel, Lutz D. (2007). "(10370) Hylonome". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 731. doi:10.1007/978-3-540-29925-7_7947. ISBN 978-3-540-00238-3.
    4. 1 2 3 4 "JPL Small-Body Database Browser: 10370 Hylonome (1995 DW2)" (2010-06-14 last obs.). Jet Propulsion Laboratory. Retrieved 5 July 2017.
    5. 1 2 John Stansberry; Will Grundy; Mike Brown; Dale Cruikshank; John Spencer; David Trilling; et al. (20 February 2007). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". arXiv:astro-ph/0702538.
    6. 1 2 3 4 5 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:1309.0946. Bibcode:2014A&A...564A..92D. doi:10.1051/0004-6361/201322377. S2CID 119177446.
    7. 1 2 3 "LCDB Data for (10370) Hylonome". Asteroid Lightcurve Database (LCDB). Retrieved 26 May 2016.
    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:1206.3153. Bibcode:2012A&A...546A..86P. doi:10.1051/0004-6361/201219057. S2CID 55876118. 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. S2CID 4313184.
    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. 1 2 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/0407400. Bibcode:2004MNRAS.354..798H. doi:10.1111/j.1365-2966.2004.08240.x. S2CID 16002759. 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 29 April 2009. Retrieved 25 April 2009.
      "The SOLEX page". Archived from the original on 29 April 2009.
    16. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 26 May 2016.
    17. ↑ Miller, Kirk; Stein, Zane (26 August 2021). "Comment on U+26B7 CHIRON" (PDF). L2/21-225.
    18. ↑ Showalter, Mark R.; Benecchi, Susan D.; Buie, Marc W.; Grundy, William M.; Keane, James T.; Lisse, Carey M.; Olkin, Cathy B.; Porter, Simon B.; Robbins, Stuart J.; Singer, Kelsi N.; Verbiscer, Anne J.; Weaver, Harold A.; Zangari, Amanda M.; Hamilton, Douglas P.; Kaufmann, David E. (2021). "A statistical review of light curves and the prevalence of contact binaries in the Kuiper Belt". Icarus. 356: 114098. arXiv:2105.03543. doi:10.1016/j.icarus.2020.114098. S2CID 225284888.
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