[Collisions, accrétion, et érosion dans la ceinture de Kuiper]
La modélisation des collisions constitue depuis presque dix ans un domaine fertile de la recherche sur la ceinture de Kuiper. Cette modélisation a fourni des résultats importants concernant les propriétés de surface des objets de la ceinture de Kuiper (KBO), la distribution en taille des KBO, leur origine, les propriétés de la ceinture de Kuiper primitive et, tout récement, la formation des satellites de KBO. Dans cet article, nous passons brièvement en revue quelques aspects particuliers de ces résultats. Farinella et al. (dans : Protostars and Planets IV, Mannings et al. (Eds.), University of Arizona Press, 2001) ont donné un traitement bien plus complet, mais antérieur, de ce sujet.
Collisional modeling has been a fertile area of Kuiper Belt research for almost a decade. Such modeling has yielded important results concerning expected KBO surface properties, the KBO size distribution, the origin of KBOs and the properties of the primoridal Kuiper Belt, and most recently, the formation of KBO satellites. In what follows we briefly review some isolated aspects of these research results. A far more comprehensive, but older review of this topic was provided by Farinella et al. (in: Protostars and Planets IV, Mannings et al. (Eds.), University of Arizona Press, 2001).
Mot clés : Ceinture de Kuiper, Collisions, Accrétion
S.Alan Stern 1 ; Scott J. Kenyon 2
@article{CRPHYS_2003__4_7_803_0, author = {S.Alan Stern and Scott J. Kenyon}, title = {Collisions, accretion, and erosion in the {Kuiper} {Belt}}, journal = {Comptes Rendus. Physique}, pages = {803--808}, publisher = {Elsevier}, volume = {4}, number = {7}, year = {2003}, doi = {10.1016/j.crhy.2003.10.008}, language = {en}, }
S.Alan Stern; Scott J. Kenyon. Collisions, accretion, and erosion in the Kuiper Belt. Comptes Rendus. Physique, Volume 4 (2003) no. 7, pp. 803-808. doi : 10.1016/j.crhy.2003.10.008. https://comptes-rendus.academie-sciences.fr/physique/articles/10.1016/j.crhy.2003.10.008/
[1] Astron. J., 110 (1995), p. 856
[2] Astron. J., 112 (1996), p. 1203
[3] Icarus, 125 (1997), p. 50
[4] Icarus, 145 (2000), p. 220
[5] Astron. J., 124 (2002), p. 2297
[6] Astron. J., 112 (1996), p. 2310
[7] Evolution of the Protoplanetary Cloud and Formation of the Earth and Planets, Nauka, Moscow, 1969 ([Translation 1972, NASA TT F-677])
[8] Icarus, 106 (1993), p. 190
[9] Icarus, 155 (2002), p. 436
[10] Astron. J., 114 (1997), p. 841
[11] Astrophys. J., 490 (1997), p. 879
[12] Astron. J., 118 (1999), p. 1101
[13] Publ. Astron. Soc. Pac., 114 (2002), p. 265
[14] Astron. J. (2004) (in preparation)
[15] Astrophys. J., 526 (1999), p. 465
[16] Annu. Rev. Astron. Astrophys., 40 (2002), p. 63
[17] Astron. J., 105 (1993), p. 1987
[18] Astrophys. J., 406 (1993), p. L35
[19] Astron. J., 111 (1996), p. 504
[20] Icarus, 128 (1997), p. 464
[21] Protostars Planets IV (V. Mannings; A.P. Boss; S.S. Russell, eds.), Univ. of Arizona, Tucson, 2000, p. 639
[22] Icarus, 251 (2001), p. 286
[23] Astrophys. J., 577 (2002), p. L35
[24] Nature, 416 (2002), p. 711
[25] Asteroids III (W. Bottke; A. Cellino; P. Paolicchi; R. Binzel, eds.), Univ. of Arizona Press, Tucson, 2002, p. 289
[26] Astron. J., 83 (1978), p. 1005
[27] Nature, 420 (2002), p. 643
[28] Icarus, 160 (2002), p. 212
[29] Pluto and Charon (S.A. Stern; D.J. Tholen, eds.), Univ. of Arizona Press, Tucson, 1997, p. 605
[30] Pluto and Charon (S.A. Stern; D.J. Tholen, eds.), Univ. of Arizona Press, Tucson, 1997, p. 159
[31] Astron. J., 124 (2002), p. 2300
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