{{Short description|Group of satellites orbiting Jupiter}} {{Use dmy dates|date=July 2022}} [[File:Carme group aei orbits polar plot.svg|thumb|upright=1.5|This diagram compares the orbital elements and relative sizes of the known members of the Carme group {{asof|April 2026|lc=y}}. The horizontal axis illustrates their average distance from Jupiter, the vertical axis their orbital inclination, and the circles their relative sizes.]] thumb|upright=1.5|107 irregular moons of Jupiter plotted by semi-major axis and inclination {{asof|April 2026|lc=y}}. The Carme group is shown as a tight cluster of red-colored points on the left.
The '''Carme group''' (or ''family'' or ''cluster''), also referred to as the '''165° inclination cluster''',<ref name="Grav2003" /> 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):<ref name="SheppardJewittPorco2004"> 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 [http://www.ifa.hawaii.edu/~jewitt/papers/JUPITER/JSP.2003.pdf Full text(pdf).] {{webarchive |url=https://web.archive.org/web/20070614045102/http://www.ifa.hawaii.edu/~jewitt/papers/JUPITER/JSP.2003.pdf |date=June 14, 2007 }}</ref><ref name="Nesvorny2004"> David Nesvorný, Cristian Beaugé, and Luke Dones''. Collisional Origin of Families of Irregular Satellites'', The Astronomical Journal, '''127''' (2004), pp. 1768–1783 [http://www.boulder.swri.edu/~davidn/papers/irrbig.pdf Full text.]</ref>
{| class="wikitable sortable" style="text-align:center;" !Name||Diameter<br>(km)<ref name="scott jupiter"/>||Semi-Major Axis<br>(km)||Period<br>(days)<ref name="nasa parameters"/>{{Efn|Negative period is indicative of retrograde motion.}}||Notes |-id=Carme |Carme || 46 || {{val|23139200}} || –719.28 || largest member and group prototype |-id=Kalyke <!-- S/2000 J 2 --> |Kalyke || 5 || {{val|23298000}} || –726.70 || substantially redder than the others |-id=Erinome <!-- S/2000 J 4 --> |Erinome || 3 || {{val|23027200}} || –714.05 || |-id=Isonoe <!-- S/2000 J 6 --> |Isonoe || 4 || {{val|22976300}} || –711.66 || |-id=Taygete <!-- S/2000 J 9 --> |Taygete || 5 || {{val|23103400}} || –717.59 || |-id=Chaldene <!-- S/2000 J 10 --> |Chaldene || 4 || {{val|22926300}} || –709.36 || |-id=Pasithee <!-- S/2001 J 6 --> |Pasithee || 2 || {{val|22840800}} || –705.41 || |-id=Kale <!-- S/2001 J 8 --> |Kale || 2 || {{val|23047800}} || –715.02 || |-id=Aitne <!-- S/2001 J 11 --> |Aitne || 3 || {{val|23059400}} || –715.54 || |-id=Arche <!-- S/2002 J 1 --> |Arche || 3 || {{val|23093200}} || –717.11 || |-id=Eukelade <!-- S/2003 J 1 --> |Eukelade || 4 || {{val|23062400}} || –715.69 || |-id=Eirene <!-- S/2003 J 5 --> |Eirene || 4 || {{val|23051300}} || –715.19 || |-id=S/2003 J 9 |S/2003 J 9 || 1 || {{val|23195100}} || –721.88 || |-id=S/2003 J 10 |S/2003 J 10 || 2 || {{val|23384400}} || –730.74 || |-id=Kallichore <!-- S/2003 J 11 --> |Kallichore || 3.8 || {{val|23017100}} || –713.59 || Possible flyby target of ''Juice'' mission |-id=Herse <!-- S/2003 J 17 --> |Herse || 2 || {{val|23146700}} || –719.63 || |-id=S/2003 J 19 |S/2003 J 19 || 2 || {{val|23153100}} || –719.92 || |-id=S/2003 J 24 |S/2003 J 24 || 2 || {{val|22882400}} || –707.33 || |-id=S/2010 J 1 |S/2010 J 1 || 2 || {{val|23185600}} || –721.43 || |-id=S/2011 J 1 |S/2011 J 1 || 2 || {{val|23120800}} || –718.42 || |-id=S/2017 J 2 |S/2017 J 2 || 2 || {{val|22949600}} || –710.42 || |-id=S/2017 J 5 |S/2017 J 5 || 2 || {{val|23202000}} || –722.20 || |-id=S/2017 J 8 |S/2017 J 8 || 1 || {{val|22819600}} || –704.42 || |-id=S/2016 J 3 |S/2016 J 3 || 2 || {{val|22719300}} || –699.76 || |-id=S/2018 J 3 |S/2018 J 3 || 1 || {{val|23400200}} || –731.49 || |-id=S/2021 J 4 |S/2021 J 4 || 1 || {{val|23019700}} || –713.71 || |-id=S/2021 J 5 |S/2021 J 5 || 2 || {{val|23414600}} || –732.15 || |-id=S/2021 J 6 |S/2021 J 6 || 1 || {{val|22870400}} || –706.77 || |-id=S/2022 J 1 |S/2022 J 1 || 2 || {{val|22744700}} || –700.93 || |-id=S/2022 J 2 |S/2022 J 2 || 1 || {{val|23073400}} || –716.21 || |-id=S/2017 J 11 |S/2017 J 11 || 2 || {{val|22991300}} || –712.38 || |-id=S/2018 J 5 |S/2018 J 5 || 2 || {{val|23269900}} || –725.38 || |-id=S/2024 J 1 |S/2024 J 1 || 2 || {{val|23462100}} || –734.38 || |-id=S/2011 J 5 |S/2011 J 5 || 2 || {{val|23527800}} || –737.46 || |-id=S/2011 J 6 |S/2011 J 6 || 1 || {{val|23238700}} || –723.93 || |-id=S/2017 J 12 |S/2017 J 12 || 1 || {{val|23270500}} || –725.40 || |-id=S/2017 J 13 |S/2017 J 13 || 1 || {{val|22842700}} || –705.50 || |-id=S/2010 J 4 |S/2010 J 4 || 1 || {{val|22793400}} || –703.19 || |-id=S/2017 J 16 |S/2017 J 16 || 1 || {{val|23007800}} || –713.13 || |-id=S/2017 J 18 |S/2017 J 18 || 2 || {{val|22923800}} || –709.24 || |-id=S/2010 J 5 |S/2010 J 5 || 1 || {{val|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{{Efn|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.}} 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).<ref name="Nesvorny2003">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. [http://www.journals.uchicago.edu/AJ/journal/issues/v126n1/202528/202528.web.pdf (pdf)] {{Webarchive|url=https://web.archive.org/web/20200415190214/http://www.journals.uchicago.edu/AJ/journal/issues/v126n1/202528/202528.web.pdf|date=15 April 2020}}</ref> 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.<ref>{{cite journal | last = Sheppard | first = Scott S. | authorlink = Scott S. Sheppard |author2=Jewitt, David C. |authorlink2=David C. Jewitt | title = An abundant population of small irregular satellites around Jupiter | journal = Nature | volume = 423 | pages = 261–263 | date = May 5, 2003 | doi = 10.1038/nature01584 | pmid = 12748634 | issue = 6937 |bibcode = 2003Natur.423..261S | s2cid = 4424447 }}</ref>
Further support to the single body origin comes from the known colours: all the satellites appear light red,{{Efn|With the exception of Kalyke, which is substantially redder.}} with colour indices B-V= 0.76 and V-R= 0.47<ref name="Grav2003">{{Cite journal |last1=Grav |first1=Tommy |last2=Holman |first2=Matthew J. |author-link2=Matthew J. Holman |last3=Gladman |first3=Brett |author-link3=Brett Gladman |last4=Aksnes |first4=Kaare |author-link4=Kaare Aksnes |date=2003-01-02 |title=Photometric Survey of the Irregular Satellites |journal=Icarus |language=en |volume=166 |issue=1 |pages=33–45 |doi=10.1016/j.icarus.2003.07.005 |arxiv=astro-ph/0301016 |bibcode=2003Icar..166...33G }}</ref> and infrared spectra, similar to D-type asteroids.<ref name="Grav2004"> {{Cite journal |last1=Grav |first1=Tommy |last2=Holman |first2=Matthew J. |author-link2=Matthew J. Holman |date=2003-12-22 |title=Near-Infrared Photometry of Irregular Satellites of Jupiter and Saturn |journal=The Astrophysical Journal |language=en |volume=605 |issue=2 |pages=L141–L144 |doi=10.1086/420881 |arxiv=astro-ph/0312571 }}</ref> These data are consistent with a progenitor from the Hilda family or a Jupiter trojan.
== Notes == <references group="lower-alpha" />
==References== {{Reflist|refs=
<ref name="nasa parameters">{{cite web |title = Planetary Satellite Mean Elements |url = https://ssd.jpl.nasa.gov/sats/elem/ |work = Jet Propulsion Laboratory |publisher = California Institute of Technology |date = 25 January 2024}}</ref>
<ref name="scott jupiter">{{cite web |title = Moons of Jupiter |url = https://sites.google.com/carnegiescience.edu/sheppard/moons/jupitermoons |work = Carnegie Science |publisher = Minor Planet Center |date = 27 August 2019}}</ref>
}}
== External links == {{Moons of Jupiter}}
{{DEFAULTSORT:Carme Group}} Category:Carme group Category:Moons of Jupiter Category:Irregular satellites Category:Moons with a retrograde orbit