234 Barbara

234 Barbara
Discovery
Discovered byC. H. F. Peters
Discovery date12 August 1883
Designations
(234) Barbara
Named after
Saint Barbara?
A883 PA, 1942 RL1
1953 RE,1975 XP
Main belt
Orbital characteristics[1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc131.26 yr (47944 d)
Aphelion2.97153 AU (444.535 Gm)
Perihelion1.79939 AU (269.185 Gm)
2.38546 AU (356.860 Gm)
Eccentricity0.24569
3.68 yr (1345.7 d)
19.28 km/s
16.9454°
0° 16m 3.05s / day
Inclination15.3746°
144.553°
192.344°
Physical characteristics
Dimensions43.75±1.0 km[1]
45.62 ± 1.93 km[2]
Mass(0.44 ± 1.45) × 1018 kg[2]
26.4744 h (1.10310 d)
0.2276±0.011
S
9.02

234 Barbara is a main belt asteroid that was discovered by German-American astronomer Christian Heinrich Friedrich Peters on August 12, 1883, in Clinton, New York. The object is orbiting the Sun with a semimajor axis of 2.385 AU, a period of 3.68 years, and an eccentricity of 0.25. The orbital plane is inclined by 15.37° to the plane of the ecliptic. It is classified as a stony S-type asteroid based upon its spectrum. The mean diameter of this object is estimated as 45.6 km.[2] It has a rotation rate of 26.5 hours, or a little over a day. It is possibly named for Saint Barbara, patron saint of mathematicians.[3][4]

Observations of light curves and stellar occultations suggest the surface exhibits large concave areas.[5] Polarimetric study of this asteroid reveals anomalous properties that suggests the regolith consists of a mixture of low and high albedo material. This may have been caused by fragmentation of an asteroid substrate with the spectral properties of CO3/CV3 carbonaceous chondrites.[6] It is the prototype for a class of asteroids called "Barbarians" that display a strong infrared absorption band at 2μm, which is a characteristic of an FeO–enriched spinel mineral. Multiple other examples of this class have since been discovered.[7]

Observations made in 2009 with ESO's Very Large Telescope Interferometer (VLTI) suggested that 234 Barbara may be a binary asteroid,[8] although a paper published in 2015 states that "the VLTI observations can be explained without the presence of a large satellite".[5]

References

  1. ^ a b Yeomans, Donald K., "234 Barbara", JPL Small-Body Database Browser, NASA Jet Propulsion Laboratory, retrieved 12 May 2016.
  2. ^ a b c 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.
  3. ^ Schmadel, Lutz (5 August 2003). Dictionary of Minor Planet Names. Springer Science & Business Media. ISBN 9783540002383 – via Google Books.
  4. ^ Paluzíe-Borrell, Antonio (11 July 1963). "The Names of the Minor Planets and Their Meanings". J. Meeus, Kesselberg Sterrenwacht – via Google Books.
  5. ^ a b Tanga, P.; et al. (April 2015), "The non-convex shape of (234) Barbara, the first Barbarian*", Monthly Notices of the Royal Astronomical Society, 448 (4): 3382–3390, arXiv:1502.00460, Bibcode:2015MNRAS.448.3382T, doi:10.1093/mnras/stv229.
  6. ^ Gil-Hutton, R.; et al. (April 2008), "New cases of unusual polarimetric behavior in asteroids", Astronomy and Astrophysics, 482 (1): 309–314, Bibcode:2008A&A...482..309G, doi:10.1051/0004-6361:20078965.
  7. ^ Devogèle, M.; et al. (April 2018), "New polarimetric and spectroscopic evidence of anomalous enrichment in spinel-bearing calcium-aluminium-rich inclusions among L-type asteroids", Icarus, 304: 31–57, arXiv:1802.06975, Bibcode:2018Icar..304...31D, doi:10.1016/j.icarus.2017.12.026, S2CID 54992862
  8. ^ "Powerful New Technique to Measure Asteroids' Sizes and Shapes". European Southern Observatory. Archived from the original on 22 December 2015. Retrieved 19 December 2015.