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 range between 22.7 and 23.6 million km, their orbital inclinations between 164.4° and 164.9°, and their orbital eccentricities between 0.25 and 0.28.
The Carme group members are :
| Name | Diameter | Semi-Major Axis | Period | Notes |
| Carme | 46 | –719.28 | largest member and group prototype | |
| Kalyke | 5 | –726.70 | substantially redder than the others | |
| Erinome | 3 | –714.05 | ||
| Isonoe | 4 | –711.66 | ||
| Taygete | 5 | –717.59 | ||
| Chaldene | 4 | –709.36 | ||
| Pasithee | 2 | –705.41 | ||
| Kale | 2 | –715.02 | ||
| Aitne | 3 | –715.54 | ||
| Arche | 3 | –717.11 | ||
| Eukelade | 4 | –715.69 | ||
| Eirene | 4 | –715.19 | ||
| S/2003 J 9 | 1 | –721.88 | ||
| S/2003 J 10 | 2 | –730.74 | ||
| Kallichore | 2 | –713.59 | ||
| Herse | 2 | –719.63 | ||
| S/2003 J 19 | 2 | –719.92 | ||
| S/2003 J 24 | 2 | –707.33 | ||
| S/2010 J 1 | 2 | –721.43 | ||
| S/2011 J 1 | 2 | –718.42 | ||
| S/2017 J 2 | 2 | –710.42 | ||
| S/2017 J 5 | 2 | –722.20 | ||
| S/2017 J 8 | 1 | –704.42 | ||
| S/2016 J 3 | 2 | –699.76 | ||
| S/2018 J 3 | 1 | –731.49 | ||
| S/2021 J 4 | 1 | –713.71 | ||
| S/2021 J 5 | 2 | –732.15 | ||
| S/2021 J 6 | 1 | –706.77 | ||
| S/2022 J 1 | 2 | –700.93 | ||
| S/2022 J 2 | 1 | –716.21 | ||
| S/2017 J 11 | 2 | –712.38 |
The International Astronomical Union reserves names ending in -e for all retrograde moons.
Origin
The very low dispersion of the mean orbital elements among the core members 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. 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: all the satellites appear light red, with colour indices B-V= 0.76 and V-R= 0.47 and infrared spectra, similar to D-type asteroids. These data are consistent with a progenitor from the Hilda family or a Jupiter trojan.