The Carme group (or family or cluster; also referred to as the 165° inclination cluster[1]) 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 164.3° and 164.9°, and their orbital eccentricities between 0.24 and 0.28.
The International Astronomical Union (IAU) reserves names ending in -e for all retrograde moons of Jupiter, which includes all those in the Carme group.
Origin
editThe very low dispersion of the mean orbital elements[a] among the core members (the group is separated by less than 900,000 km in semi major axis and only 0.6° 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).[2] 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.[3]
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[1] and infrared spectra, similar to D-type asteroids.[4] These data are consistent with a progenitor from the Hilda family or a Jupiter trojan.[1] However, one moon, Kalyke, is substantially redder, consistent with the colour of a centaur or a Trans-Neptunian object instead. As such it was suggested it may have its origin somewhere else, an interloper from the outer Solar System.[1][5] Alternatively, Kalyke might be a remnant of the object that collided with the Carme group progenitor, as opposed to being a fragment of the progenitor itself. However, it would be unusual for such a remnant to settle into a post-collision orbit very similar to the progenitor it impacted.[1]
List
editThe Carme group members are (in order by date announcement):[6][7]
| Name | Diameter (km)[8][9] | Semi-Major Axis (km)[10] | Period (days)[10][b] | Notes |
|---|---|---|---|---|
| Carme | 46.7 | 23139200 | –719.28 | largest member and group prototype |
| Kalyke | 6.9 | 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 | |
| Jupiter LXI | 2 | 23153100 | –719.92 | |
| S/2003 J 24 | 2 | 22882400 | –707.33 | |
| Jupiter LI | 2 | 23185600 | –721.43 | |
| Jupiter LXXII | 2 | 23120800 | –718.42 | |
| Jupiter LXIII | 2 | 22949600 | –710.42 | |
| Jupiter LXVI | 2 | 23202000 | –722.20 | |
| Jupiter LXIX | 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 |
Notes
edit- ↑ 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.
- ↑ Negative period is indicative of retrograde motion.
References
edit- 1 2 3 4 5 Grav, Tommy; Holman, Matthew J.; Gladman, Brett; Aksnes, Kaare (November 2003). "Photometric Survey of the Irregular Satellites". Icarus. 166 (1): 33–45. arXiv:astro-ph/0301016. Bibcode:2003Icar..166...33G. doi:10.1016/j.icarus.2003.07.005. S2CID 15665146.
- ↑ Nesvorný, David; Alvarellos, Jose L. A.; Dones, Luke; Levison, Harold F. (July 2003). "Orbital and Collisional Evolution of the Irregular Satellites". The Astronomical Journal. 126 (1): 398–429. Bibcode:2003AJ....126..398N. doi:10.1086/375461. ISSN 0004-6256.
- ↑ Sheppard, Scott S.; Jewitt, David C. (5 May 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. (April 2004). "Near-Infrared Photometry of Irregular Satellites of Jupiter and Saturn". The Astrophysical Journal. 605 (2): L141–L144. arXiv:astro-ph/0312571. Bibcode:2004ApJ...605L.141G. doi:10.1086/420881. S2CID 15665146.
- ↑ Vilas, Faith; Lederer, Susan M.; Gill, Sara L.; Jarvis, Kandy S.; Thomas-Osip, Joanna E. (February 2006). "Aqueous alteration affecting the irregular outer planets satellites: Evidence from spectral reflectance". Icarus. 180 (2): 453–463. Bibcode:2006Icar..180..453V. doi:10.1016/j.icarus.2005.10.004.
- ↑ Sheppard, Scott S.; Jewitt, David C.; Porco, Carolyn (2004). "Jupiter's outer satellites and Trojans" (PDF). In Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (eds.). Jupiter. The planet, satellites and magnetosphere. Cambridge planetary science. Vol. 1. Cambridge, UK: Cambridge University Press. pp. 263–280. Bibcode:2004jpsm.book..263J. ISBN 0-521-81808-7. S2CID 117582048. Archived from the original (PDF) on 14 June 2007.
- ↑ Nesvorný, David; Beaugé, Cristian; Dones, Luke (March 2004). "Collisional Origin of Families of Irregular Satellites". The Astronomical Journal. 127 (3): 1768–1783. Bibcode:2004AJ....127.1768N. doi:10.1086/382099. ISSN 0004-6256.
- ↑ Grav, T.; Bauer, J. M.; Mainzer, A. K.; Masiero, J. R.; Nugent, C. R.; Cutri, R. M.; et al. (August 2015). "NEOWISE: Observations of the Irregular Satellites of Jupiter and Saturn". The Astrophysical Journal. 809 (1): 9. arXiv:1505.07820. Bibcode:2015ApJ...809....3G. doi:10.1088/0004-637X/809/1/3. S2CID 5834661. 3.
- ↑ "Moons of Jupiter". Carnegie Science. Minor Planet Center. 27 August 2019.
- 1 2 "Planetary Satellite Mean Elements". Jet Propulsion Laboratory. California Institute of Technology. 25 January 2024.