354 Eleonora

354 Eleonora
Discovery
Discovered byAuguste Charlois
Discovery date17 January 1893
Designations
(354) Eleonora
Pronunciation/ɛliəˈnɔːrə/[1]
1893 A
Main belt
AdjectivesEleonorian
Orbital characteristics[2]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc123.16 yr (44983 d)
Aphelion3.1188 AU (466.57 Gm)
Perihelion2.47676 AU (370.518 Gm)
2.79777 AU (418.540 Gm)
Eccentricity0.11474
4.68 yr (1709.3 d)
123.762°
0° 12m 38.196s / day
Inclination18.403°
140.37°
5.5215°
Physical characteristics
Dimensions0.25[a]
165±3 km[3]
154.3±5.6 km[4]
148.970±0.425 km[5][2]
Mass(7.5±2.7)×1018 kg[3]
(7.18±2.57)×1018 kg[4]
(6.236 ± 1.305/1.214)×1018 kg[5]
Mean density
3.18±1.14 g/cm3[3]
3.73±1.39 g/cm3[4]
3.602 ± 0.754/0.701 g/cm3[5]
4.277 h (0.1782 d)[2]
0.172[3]
0.201±0.052[2]
S
6.15[2]

354 Eleonora is a large, stony main-belt asteroid that was discovered by the French astronomer Auguste Charlois on January 17, 1893, in Nice.[6]

Photometric observations of this asteroid gave a light curve with a period of 13.623 hours. The data was used to construct a model for the asteroid, revealing it to be a regular-shaped object, spinning about a pole with ecliptic coordinates (β, λ) = (+20°, 356°), although this is with an accuracy of only ±10°. The ratio of the major to minor axes lengths is roughly equal to 1.2.[7] It is classified as an S-type asteroid and has an estimated size of 154.34 km.[4] The spectrum of 354 Eleonora reveals the strong presence of the mineral olivine, a relative rarity in the asteroid belt.[8]

During favorable oppositions, such as in 1968 and 2010, Eleonora can reach an apparent magnitude of +9.31.

Notes

  1. ^ Flattening derived from the maximum aspect ratio (c/a): , where (c/a) = 0.75±0.08.[3]

References

  1. ^ "Eleonora". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  2. ^ a b c d e Yeomans, Donald K., "354 Eleonora", JPL Small-Body Database Browser, NASA Jet Propulsion Laboratory, retrieved 11 May 2016.
  3. ^ a b c d e P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
  4. ^ a b c d Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, 73 (1): 98–118, arXiv:1203.4336, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009, S2CID 119226456. See Table 1.
  5. ^ a b c Fienga, A.; Avdellidou, C.; Hanuš, J. (February 2020). "Asteroid masses obtained with INPOP planetary ephemerides". Monthly Notices of the Royal Astronomical Society. 492 (1). doi:10.1093/mnras/stz3407.
  6. ^ "Numbered Minor Planets 1–5000", Discovery Circumstances, IAU Minor Planet center, retrieved 7 April 2013.
  7. ^ Kaasalainen, M.; et al. (October 2002), "Models of Twenty Asteroids from Photometric Data", Icarus, 159 (2): 369–395, Bibcode:2002Icar..159..369K, doi:10.1006/icar.2002.6907.
  8. ^ Burbine, T. H.; et al. (July 2000), "The Nature of Olivine Asteroids", Meteoritics & Planetary Science, vol. 35, pp. A35, Bibcode:2000M&PSA..35R..35B, doi:10.1111/j.1945-5100.2000.tb01796.x.


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