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The Carme group is a group of retrograde irregular satellites of Jupiter that follow similar orbits to Carme and are thought to have a common origin. Their semi-major axes (distances from Jupiter) range between 22.9 and 24.1 Gm, their orbital inclinations between 164.9° and 165.5°, and their orbital eccentricities between 0.23 and 0.27 (with one exception). The core members include (from largest to smallest):〔 Scott S. Sheppard, David C. Jewitt, Carolyn Porco ''Jupiter's outer satellites and Trojans'', In: ''Jupiter. The planet, satellites and magnetosphere.'' Edited by Fran Bagenal, Timothy E. Dowling, William B. McKinnon. Cambridge planetary science, Vol. 1, Cambridge, UK: Cambridge University Press, ISBN 0-521-81808-7, 2004, p. 263 - 280 (Full text(pdf). )〕〔 David Nesvorný, Cristian Beaugé, and Luke Dones ''Collisional Origin of Families of Irregular Satellites'', The Astronomical Journal, 127 (2004), pp. 1768–1783 (Full text. )〕 * Carme (the largest, which gives its name to the group) * Taygete * Eukelade〔Listed by Nesvorny 2004 as a ''possible'' member, not listed by Sheppard 2004; the orbital elements confirmed by Jacobson 2004〕 * S/2003 J 5〔 * Chaldene * Isonoe * Kalyke (substantially redder than the others) * Erinome * Aitne * Kale * Pasithee * S/2003 J 9〔 * S/2003 J 10〔 The International Astronomical Union (IAU) reserves names ending in -e for all retrograde moons, including this group's members. ==Origin== The very low dispersion of the mean1 orbital elements among the core members (the group is separated by less than 700,000 km in semi major axis and less than 0.7° in inclination) suggests that the Carme group may once have been a single body that was broken apart by an impact. The dispersion can be explained by a very small velocity impulse (5 < δV < 50 m/s).〔David Nesvorný, Jose L. A. Alvarellos, Luke Dones, and Harold F. Levison ''Orbital and Collisional Evolution of the Irregular Satellites'', The Astronomical Journal,126 (2003), pages 398–429. ((pdf) )〕 The parent body was probably about the size of Carme, 46 km in diameter; 99% of the group's mass is still located in Carme. Further support to the single body origin comes from the known colours: all2 the satellites appear light red, with colour indices B-V= 0.76 and V-R= 0.47〔Grav, Tommy; Holman, Matthew J.; Gladman, Brett J.; Aksnes, Kaare ''Photometric survey of the irregular satellites'', Icarus, 166,(2003), pp. 33-45. (Preprint )〕 and infrared spectra, similar to D-type asteroids.〔 Tommy Grav and Matthew J. Holman ''Near-Infrared Photometry of the Irregular Satellites of Jupiter and Saturn'',The Astrophysical Journal, 605, (2004), pp. L141–L144 (Preprint )〕 These data are consistent with a progenitor from the Hilda family or a Jupiter Trojan. 1Osculating orbital parameters of irregular satellites of Jupiter change widely in short intervals due to heavy perturbation by Jupiter. For example, changes of as much as 1 Gm in semi-major axis in 2 years, 0.5 in eccentricity in 12 years, and as much as 5° in 24 years have been reported. Mean orbital elements are the averages calculated by the numerical integration of current elements over a long period of time, used to determine the dynamical families. 2With the exception of Kalyke, substantially redder. 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Carme group」の詳細全文を読む スポンサード リンク
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