108 Hecuba

108 Hecuba
Discovery
Discovered by R. Luther
Discovery date 2 April 1869
Designations
Named after
 Hecuba
Main belt
Orbital characteristics[1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc 135.87 yr (49628 d)
Aphelion 3.4190 AU (511.48 Gm)
Perihelion 3.05922 AU (457.653 Gm)
3.23912 AU (484.565 Gm)
Eccentricity 0.055539
5.83 yr (2129.3 d)
166.649°
0° 10m 8.648s / day
Inclination 4.2204°
350.014°
204.634°
Earth MOID 2.05833 AU (307.922 Gm)
Jupiter MOID 1.55152 AU (232.104 Gm)
Jupiter Tisserand parameter 3.178
Physical characteristics
Dimensions 64.97±4.4 km[1]
65 km[2]
Mass ~3.9×1017 kg (estimate)
Mean density
 ~2.7 g/cm³ (estimate)[3]
Equatorial escape velocity
 ~0.040 km/s (estimate)
14.256 h (0.5940 d)[1]
0.60 d or 1.20 d[4]
0.2431±0.037
Surface temp. min mean max
Kelvin ~148 215
Celsius -58
S[5]
8.09

    108 Hecuba is a fairly large and bright main-belt asteroid. It was discovered by Karl Theodor Robert Luther on April 2, 1869,[6] and named after Hecuba, wife of King Priam in the legends of the Trojan War in Greek Mythology. It became the first asteroid discovered to orbit near a 2:1 mean-motion resonance with the planet Jupiter,[7] and is the namesake of the Hecuba group of asteroids.[8]

    In the Tholen classification system, it is categorized as a stony S-type asteroid, while the Bus asteroid taxonomy system lists it as an Sw asteroid.[9] Observations performed at the Palmer Divide Observatory in Colorado Springs, Colorado in during 2007 produced a light curve with a period of 17.859 ± 0.005 hours with a brightness range of 0.11 ± 0.02 in magnitude.[10]

    Hecuba orbits within the Hygiea family of asteroids but is not otherwise related to other family members because it has a silicate composition; Hygieas are dark C-type asteroids.

    References

    1. 1 2 3 Yeomans, Donald K., "108 Hecuba", JPL Small-Body Database Browser, NASA Jet Propulsion Laboratory, retrieved 12 May 2016.
    2. ↑ "Archived copy". Archived from the original on 2005-12-11. Retrieved 2005-12-11.
    3. ↑ Krasinsky, G. A.; et al. (July 2002), "Hidden Mass in the Asteroid Belt", Icarus, 158 (1): 98–105, Bibcode:2002Icar..158...98K, doi:10.1006/icar.2002.6837. See appendix A.
    4. ↑ Harris, A.W.; Warner, B.D.; Pravec, P., eds. (2012), "Lightcurve Derived Data", Planetary Data System, NASA, retrieved 2013-03-22.
    5. ↑ DeMeo, Francesca E.; et al. (2011), "An extension of the Bus asteroid taxonomy into the near-infrared" (PDF), Icarus, 202 (1): 160–180, Bibcode:2009Icar..202..160D, doi:10.1016/j.icarus.2009.02.005. See appendix A.
    6. ↑ "Numbered Minor Planets 1–5000", Discovery Circumstances, IAU Minor Planet center, retrieved 2013-04-07.
    7. ↑ Brož, M.; Vokrouhlický, D.; Roig, F.; Nesvorný, D.; Bottke, W. F.; Morbidelli, A. (June 2005), "Yarkovsky origin of the unstable asteroids in the 2/1 mean motion resonance with Jupiter", Monthly Notices of the Royal Astronomical Society, 359 (4), Bibcode:2005MNRAS.359.1437B, doi:10.1111/j.1365-2966.2005.08995.x.
    8. ↑ McDonald, Sophia Levy (June 1948), "General perturbations and mean elements, with representations of 35 minor planets of the Hecuba group", Astronomical Journal, 53, p. 199, Bibcode:1948AJ.....53..199M, doi:10.1086/106097.
    9. ↑ DeMeo, Francesca E.; et al. (July 2009), "An extension of the Bus asteroid taxonomy into the near-infrared" (PDF), Icarus, 202 (1), pp. 160–180, Bibcode:2009Icar..202..160D, doi:10.1016/j.icarus.2009.02.005, retrieved 2013-04-08. See appendix A.
    10. ↑ Warner, Brian D. (September 2007), "Asteroid Lightcurve Analysis at the Palmer Divide Observatory", The Minor Planet Bulletin, Bibcode:2007MPBu...34...72W.

    External links


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