Carme group
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 (negative period indicates retrograde orbit):[1][2]
Name | Diameter (km) |
Period (days) |
Notes |
---|---|---|---|
Carme | 46.7 | −693.17[3] | largest member and group prototype |
Taygete | 5 | −691.62[4] | |
Eukelade[5] | 4 | −693.02[3] | |
Eirene[5] | 3 | −743.88[6] | |
Chaldene | 4 | −759.88[7] | |
Isonoe | 4 | −688.61[7] | |
Kalyke | 6.9 | −766.61[7] | substantially redder than the others |
Erinome | 3 | −682.80[3] | |
Aitne | 3 | −712.04[7] | |
Kale | 2 | −736.55[3] | |
Pasithee | 2 | −711.12[3] | |
S/2003 J 9 (probably)[5] | 1 | −767.60[8] |
The International Astronomical Union (IAU) reserves names ending in -e for all retrograde moons.
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).[9] 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.[10]
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[11] and infrared spectra, similar to D-type asteroids.[12] 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 the Sun. 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.
References[]
- ^ 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). Archived June 14, 2007, at the Wayback Machine
- ^ David Nesvorný, Cristian Beaugé, and Luke Dones Collisional Origin of Families of Irregular Satellites, The Astronomical Journal, 127 (2004), pp. 1768–1783 Full text.
- ^ a b c d e "M.P.C. 127087-127088" (PDF). Minor Planet Circular. Minor Planet Center. 17 November 2020.
- ^ "M.P.C. 110499" (PDF). Minor Planet Circular. Minor Planet Center. 29 May 2018.
- ^ a b c Listed by Nesvorný 2004 as a possible member, not listed by Sheppard 2004; the orbital elements confirmed by Jacobson 2004
- ^ "M.P.C. 115250" (PDF). Minor Planet Circular. Minor Planet Center. 9 June 2017.
- ^ a b c d "M.P.C. 115890-115891" (PDF). Minor Planet Circular. Minor Planet Center. 27 August 2019.
- ^ "MPEC 2020-V19 : S/2003 J 9". Minor Planet Electronic Circular. Minor Planet Center. 5 November 2020. Retrieved 5 November 2020.
- ^ 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)
- ^ Sheppard, Scott S.; Jewitt, David C. (May 5, 2003). "An abundant population of small irregular satellites around Jupiter". Nature. 423 (6937): 261–263. Bibcode:2003Natur.423..261S. doi:10.1038/nature01584. PMID 12748634. S2CID 4424447.
- ^ Grav, Tommy; Holman, Matthew J.; Gladman, Brett J.; Aksnes, Kaare Photometric survey of the irregular satellites, Icarus, 166,(2003), pp. 33-45. Preprint
- ^ 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
- Carme group
- Moons of Jupiter
- Irregular satellites