Carme group
Group of satellites orbiting Jupiter
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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 22.7 and 23.6 million km, their orbital inclinations between 164.4° and 164.9°, and their orbital eccentricities between 0.25 and 0.28 (with one exception).
The Carme group members are (in order by date announcement):[1][2]
| Name | Diameter (km)[3] | Semi-Major Axis (km) | Period (days)[4][a] | Notes |
|---|---|---|---|---|
| Carme | 46 | 23139200 | –719.28 | largest member and group prototype |
| Kalyke | 5 | 23298000 | –726.70 | substantially redder than the others |
| Erinome | 3 | 23027200 | –714.05 | |
| Isonoe | 4 | 22976300 | –711.66 | |
| Taygete | 5 | 23103400 | –717.59 | |
| Chaldene | 4 | 22926300 | –709.36 | |
| Pasithee | 2 | 22840800 | –705.41 | |
| Kale | 2 | 23047800 | –715.02 | |
| Aitne | 3 | 23059400 | –715.54 | |
| Arche | 3 | 23093200 | –717.11 | |
| Eukelade | 4 | 23062400 | –715.69 | |
| Eirene | 4 | 23051300 | –715.19 | |
| S/2003 J 9 | 1 | 23195100 | –721.88 | |
| S/2003 J 10 | 2 | 23384400 | –730.74 | |
| Kallichore | 3.8 | 23017100 | –713.59 | Possible flyby target of Juice mission |
| Herse | 2 | 23146700 | –719.63 | |
| S/2003 J 19 | 2 | 23153100 | –719.92 | |
| S/2003 J 24 | 2 | 22882400 | –707.33 | |
| S/2010 J 1 | 2 | 23185600 | –721.43 | |
| S/2011 J 1 | 2 | 23120800 | –718.42 | |
| S/2017 J 2 | 2 | 22949600 | –710.42 | |
| S/2017 J 5 | 2 | 23202000 | –722.20 | |
| S/2017 J 8 | 1 | 22819600 | –704.42 | |
| S/2016 J 3 | 2 | 22719300 | –699.76 | |
| S/2018 J 3 | 1 | 23400200 | –731.49 | |
| S/2021 J 4 | 1 | 23019700 | –713.71 | |
| S/2021 J 5 | 2 | 23414600 | –732.15 | |
| S/2021 J 6 | 1 | 22870400 | –706.77 | |
| S/2022 J 1 | 2 | 22744700 | –700.93 | |
| S/2022 J 2 | 1 | 23073400 | –716.21 | |
| S/2017 J 11 | 2 | 22991300 | –712.38 | |
| S/2018 J 5 | 2 | 23269900 | –725.38 | |
| S/2024 J 1 | 2 | 23462100 | –734.38 | |
| S/2011 J 5 | 2 | 23527800 | –737.46 | |
| S/2011 J 6 | 1 | 23238700 | –723.93 | |
| S/2017 J 12 | 1 | 23270500 | –725.40 | |
| S/2017 J 13 | 1 | 22842700 | –705.50 | |
| S/2010 J 4 | 1 | 22793400 | –703.19 | |
| S/2017 J 16 | 1 | 23007800 | –713.13 | |
| S/2017 J 18 | 2 | 22923800 | –709.24 | |
| S/2010 J 5 | 1 | 23581000 | –739.99 |
The International Astronomical Union (IAU) reserves names ending in -e for all retrograde moons.
Origin
The very low dispersion of the mean orbital elements[b] among the core members (the group is separated by less than 900,000 km in semi major axis and only 0.5° 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).[5] 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.[6]
Further support to the single body origin comes from the known colours: all the satellites appear light red,[c] with colour indices B-V= 0.76 and V-R= 0.47[7] and infrared spectra, similar to D-type asteroids.[8] These data are consistent with a progenitor from the Hilda family or a Jupiter trojan.
Notes
- Negative period is indicative of retrograde motion.
- Osculating 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 million km 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.
- With the exception of Kalyke, which is substantially redder.