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36 Atalante

From Wikipedia, the free encyclopedia
Main-belt asteroid

36 Atalante
Three-dimensional model of 36 Atalante created based on light-curve
Discovery[1]
Discovered byH. Goldschmidt
Discovery dateOctober 5, 1855
Designations
Designation
(36) Atalante
Pronunciation/ætəˈlæntə/ forAtalanta,/ætəˈlæntiː/ forAtalante[2][a]
Named after
Atalanta
A901 SB; A912 HC
Atalanta[3]
Main belt
AdjectivesAtalantean/ˌætəlænˈtiːən/[4]
Orbital characteristics
Epoch December 31, 2006 (JD 2454100.5)
Aphelion535.625 Gm (3.580 AU)
Perihelion286.217 Gm (1.913 AU)
410.921 Gm (2.747AU)
Eccentricity0.303
1662.831 d (4.55a)
17.55 km/s
47.005°
Inclination18.432°
358.472°
47.132°
Physical characteristics
132.842 ± 29.191 km[1]
110.14 ± 4.38 km[5]
Mass(9.57 ± 4.32/3.15)×1017 kg[6]
1.672 ± 0.755/0.551 g/cm3[6][b]
~0.0241 m/s²
~0.0498 km/s
0.414 d (9.93 h)[1]
Albedo0.029[1]
Temperature~170K
Spectral type
C[1]
8.59[1]

36 Atalante is a large, darkmain-beltasteroid. It was discovered by the German-French astronomerH. Goldschmidt on October 5, 1855, and named by French mathematicianUrbain Le Verrier after theGreek mythological heroineAtalanta (of whichAtalante is the French and German form, pronounced nearly the same as 'Atalanta' in English).[7] It was rendered 'Atalanta' in English sources in the 19th century.[3] This asteroid is classified as C-type (carbonaceous), according to theTholen classification system.[1]

Observation of the asteroidlight curve indicates it is rotating with a period of9.93 ± 0.01 hours. During this interval, the magnitude varies by an amplitude of 0.12 ± 0.02.[8] By combining the results of multiple light curves, the approximateellipsoidal shape of the object can be estimated. It appears to be slightly elongated, being about 28.2% longer along one axis compared to the other two.[9] Atalante was observed byAreciboradar in October 2010.[10][11]

This asteroid shares amean-motion resonance with the planetsJupiter andSaturn. The computedLyapunov time for this asteroid is only 4,000 years, indicating that it occupies a highly chaotic orbit that will change randomly over time because ofgravitational perturbations of the planets. This is the shortest Lyapunov time of the first 100 named asteroids.[12]

Notes

[edit]
  1. ^The/ætəˈlæntiː/ pronunciation is for the Greek form Ἀταλάντη; however, the nameAtalante here is actually the German form of the LatinAtalanta, with the German final -e being a schwa much like an English final -a – and indeed, 'Atalanta' is given as the English form in Craig (1869).[3]
  2. ^Assuming a diameter of 103 ± 11.451 km.

References

[edit]
  1. ^abcdefg"JPL Small-Body Database Browser: 36 Atalante" (2011-12-30 last obs).Jet Propulsion Laboratory. Retrieved23 January 2012.
  2. ^'Atalanta, Atalante' inThe Century Dictionary and Cyclopedia.
  3. ^abcJohn Craig (1869)The Universal English Dictionary
  4. ^E.g. John Milton (1749)Paradise Lost
  5. ^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.
  6. ^abFienga, A.; Avdellidou, C.; Hanuš, J. (February 2020)."Asteroid masses obtained with INPOP planetary ephemerides"(PDF).Monthly Notices of the Royal Astronomical Society.492 (1).doi:10.1093/mnras/stz3407.
  7. ^Schmadel, Lutz D.; International Astronomical Union (2003),Dictionary of minor planet names, Physics and astronomy online library, vol. 1 (5th ed.), Springer, p. 18,ISBN 3-540-00238-3
  8. ^Brinsfield, James W. (September 2007), "The Rotation Periods of 36 Atalante and 416 Vaticana",The Minor Planet Bulletin,34 (3):58–59,Bibcode:2007MPBu...34...58B
  9. ^Blanco, C.; Riccioli, D. (September 1998), "Pole coordinates and shape of 30 asteroids",Astronomy and Astrophysics Supplement,131 (3):385–394,Bibcode:1998A&AS..131..385B,doi:10.1051/aas:1998277
  10. ^Mike Nolan (18 January 2012)."Scheduled Arecibo Radar Asteroid Observations". Planetary Radar at Arecibo Observatory. Retrieved23 January 2012.
  11. ^"Radar-Detected Asteroids and Comets". NASA/JPL Asteroid Radar Research. Retrieved23 January 2012.
  12. ^Šidlichovský, M. (1999), Svoren, J.; Pittich, E. M.; Rickman, H. (eds.), "Resonances and chaos in the asteroid belt",Evolution and source regions of asteroids and comets : proceedings of the 173rd colloquium of the International Astronomical Union, held in Tatranska Lomnica, Slovak Republic, August 24–28, 1998, pp. 297–308,Bibcode:1999esra.conf..297S.

External links

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