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38 Leda

From Wikipedia, the free encyclopedia
Main-belt asteroid
For other uses of "Leda", seeLeda.

38 Leda
A three-dimensional model of 38 Leda based on its light curve
Discovery
Discovered byJ. Chacornac
Discovery dateJanuary 12, 1856
Designations
Designation
(38) Leda
Pronunciation/ˈliːdə/[1]
Named after
Leda
A904 SF;1949 QO2
Main belt
AdjectivesLedean/lɪˈdiːən/ (LatinLēdæ-us)
Orbital characteristics
Epoch December 31, 2006 (JD 2454100.5)
Aphelion472.587 Gm (3.159 AU)
Perihelion348.232 Gm (2.328 AU)
410.409 Gm (2.743AU)
Eccentricity0.152
1659.725 d (4.54a)
17.88 km/s
107.567°
Inclination6.955°
295.890°
168.804°
Physical characteristics
Dimensions92.255 ± 0.490 km[2]
Mass(7.16 ± 3.38/2.24)×1017 kg[3]
1.743 ± 0.822/0.544 g/cm3[3]
0.0225 m/s²
0.0455 km/s
0.5350 d (12.84 h)[2]
Albedo0.055[2]
Temperature~170K
Spectral type
C[2]
8.32

38 Leda is a large, darkmain-beltasteroid that was discovered by French astronomerJ. Chacornac on January 12, 1856, and named afterLeda, the mother ofHelen of Troy inGreek mythology. In theTholen classification system, it is categorized as a carbonaceousC-type asteroid, while the Busasteroid taxonomy system lists it as a Cgh asteroid.[4] The spectra of the asteroid displays evidence of aqueous alteration.[5]

Leda has been studied byradar.[6] During 2002, 38 Leda was observed by radar from theArecibo Observatory. The return signal matched an effective diameter of 116 ± 13 km. This is consistent with some asteroid dimensions computed through other means.[7][8] Based upon alight curve that was generated fromphotometric observations of this asteroid atPulkovo Observatory, it has a rotation period of 12.834 ± 0.001 hours and varies in brightness by 0.15 ± 0.01 inmagnitude.[9]

References

[edit]
  1. ^Noah Webster (1884)A Practical Dictionary of the English Language
  2. ^abcd"38 Leda".JPL Small-Body Database.Jet Propulsion Laboratory. SPK-ID: 38. Retrieved15 June 2008.
  3. ^abFienga, A.; Avdellidou, C.; Hanuš, J. (February 2020)."Asteroid masses obtained with INPOP planetary ephemerides".Monthly Notices of the Royal Astronomical Society.492 (1):589–602.doi:10.1093/mnras/stz3407.
  4. ^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, archived fromthe original(PDF) on 17 March 2014, retrieved12 April 2013. See appendix A.
  5. ^Fornasier, S.; et al. (February 1999), "Spectroscopic comparison of aqueous altered asteroids with CM2 carbonaceous chondrite meteorites",Astronomy and Astrophysics Supplement,135: 65−73,Bibcode:1999A&AS..135...65F,doi:10.1051/aas:1999161.
  6. ^"Radar-Detected Asteroids and Comets". NASA/JPL Asteroid Radar Research. Retrieved30 October 2011.
  7. ^Magri, Christopher; et al. (January 2007), "A radar survey of main-belt asteroids: Arecibo observations of 55 objects during 1999–2003",Icarus,186 (1):126–151,Bibcode:2007Icar..186..126M,doi:10.1016/j.icarus.2006.08.018
  8. ^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. See Table 1.
  9. ^Pilcher, Frederick (October 2011), "Rotation Period Determinations for 11 Parthenope, 38 Leda, 111 Ate 194 Prokne, 217 Eudora, and 224 Oceana",The Minor Planet Bulletin,38 (4):183–185,Bibcode:2011MPBu...38..183P.

External links

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