(24) Thémis

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(24) Thémis
(24) Themis
Description de cette image, également commentée ci-après
Reconstitution de la forme de l'astéroïde par inversion de sa courbe de lumière.
Caractéristiques orbitales
Époque (JJ 2453600.5)
Établi sur ?
 observ. couvrant ? (U = 0)
Demi-grand axe (a) 468,226 × 106 km
(3,130 ua)
Périhélie (q) 406,202 × 106 km
(2,715 ua)
Aphélie (Q) 530,250 × 106 km
(3,545 ua)
Excentricité (e) 0,132
Période de révolution (Prév) 2 022,486 j
(5,537 a)
Vitesse orbitale moyenne (vorb) 16,76 km/s
Inclinaison (i) 0,760°
Longitude du nœud ascendant (Ω) 35,992°
Argument du périhélie (ω) 107,989°
Anomalie moyenne (M0) 185,968°
Catégorie ceinture d'astéroïdes
(Thémis)
Caractéristiques physiques
Dimensions 198,0 km
Masse (m) 1,13±0,43 × 1019
ou 2,3 × 1019 kg[1],[2]
Masse volumique (ρ) 2 780±1 350 kg/m3
Période de rotation (Prot) 0,348 9 j
(8,374 h)
Classification spectrale C
Magnitude absolue (H) 7,08
Albédo (A) 0,067
Température (T) ~159 K

Découverte
Date
Découvert par Annibale De Gasparis
Nommé d'après Thémis
Désignation 1947 BA, 1955 OH

modifier

(24) Thémis (désignation internationale (24) Themis) est un gros astéroïde de la ceinture principale, découvert par Annibale De Gasparis le . C'est le plus grand astéroïde de la famille de Thémis. Il s'agit d'un rocher d'environ 200 kilomètres de long situé à près de 500 millions de kilomètres de la Terre[3].

Le , l'Infrared Telescope Facility de la NASA a confirmé la présence de glace d'eau sur l'ensemble de sa surface. Comme cette glace subit en permanence une légère sublimation, on suppose qu'elle se renouvelle depuis un réservoir souterrain. Des composés organiques ont également été détectés à sa surface, notamment des hydrocarbures aromatiques polycycliques, méthyles et méthylènes[4],[5],[6].

Une explication alternative de la présence de cette glace est similaire à un des scénarios de la formation d'eau sur la surface lunaire. Le bombardement de protons du vent solaire sur les oxydes minéraux de la surface formerait des hydroxyles qui se réarrangeraient en libérant des molécules d'eau[6].

Références

  1. ↑ (en) James Baer et Steven R. Chesley, « Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris », Celestial Mech Dyn Astr, Springer Science+Business Media, vol. 100,‎ , p. 27-42 (DOI 10.1007/s10569-007-9103-8, lire en ligne [PDF]).
  2. ↑ (en) G. Michalak, « Determination of asteroid masses », Astronomy & Astrophysics, Springer Science+Business Media, vol. 374,‎ , p. 703-711 (DOI 10.1051/0004-6361:20010731)
  3. ↑ L'origine extraterrestre de l'eau se confirme.
  4. ↑ (en) Ron Cowen, « Ice confirmed on an asteroid : Frozen water leaves its signature over the entire surface of the asteroid 24 Themis », Science News, vol. 176, no 10,‎ , p. 9 (lire en ligne).
  5. ↑ Andrew S. Rivkin et Joshua P. Emery, « Detection of ice and organics on an asteroidal surface », Nature, vol. 464, no 7293,‎ , p. 1322-1323 (ISSN 0028-0836, DOI 10.1038/nature09028, lire en ligne)
    accès payant
    .
  6. ↑ a et b Nancy Atkinson, « More Water Out There, Ice Found on an Asteroid », sur spacefellowship.com, (consulté le ).

Voir aussi

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