Ananke group

The Ananke group is a group of retrograde irregular satellites of Jupiter that follow similar orbits to Ananke and are thought to have a common origin.

This diagram illustrates the largest irregular satellites of Jupiter. The location of the Ananke group is illustrated by Ananke's presence near the bottom. An object's position on the horizontal axis indicates its distance from Jupiter. The vertical axis indicates its inclination. Eccentricity is indicated by yellow bars illustrating the object's maximum and minimum distances from Jupiter. Circles illustrate an object's size in comparison to the others.

Their semi-major axes (distances from Jupiter) range between 19.2 and 21.8 Gm, their orbital inclinations between 144.3° and 155.5°, and their orbital eccentricities between 0.09 and 0.30.

The members of the Ananke group are:^[1][2]

Name	Diameter (km)[3]	Period (days)[4][lower-alpha 1]
Ananke	28	–629.79
Harpalyke	4	–623.32
Iocaste	5	–631.59
Praxidike	7	–625.39
Thyone	4	–627.18
Hermippe	4	–633.90
Euanthe	3	–620.44
Euporie	2	–550.69
Orthosie	2	–622.59
Mneme	2	–620.07
Thelxinoe	2	–628.03
Helike	4	–626.33
S/2010 J 2	1	–618.84
S/2016 J 1	1	–618.49
S/2003 J 18	2	–598.12
Eupheme	2	–617.73
S/2017 J 3	2	–625.60
S/2017 J 7	2	–626.56
S/2017 J 9	3	–666.11
S/2003 J 2	2	–628.79
S/2003 J 12	1	–627.24
S/2003 J 16	2	–622.88
S/2021 J 1	1	–627.14
S/2021 J 2	1	–625.14
S/2021 J 3	2	–618.33
S/2022 J 3	1	–630.67

The International Astronomical Union (IAU) reserves names ending in -e for all retrograde moons, including this group's members.

Origin

The Ananke group is believed to have been formed when an asteroid was captured by Jupiter and subsequently fragmented by a collision. This belief is founded on the fact that the dispersion of the mean orbital parameters^{[lower-alpha 2]} of the core members is very small and can be accounted for by a small velocity impulse (15 < δV < 80 m/s), compatible with a single collision and breakup.^[5]

Based on the sizes of the satellites, the original asteroid may have been about 28 km in diameter. Since this value is near the approximate diameter of Ananke itself, it is likely the parent body was not heavily disrupted.^[6]

Available photometric studies put this in doubt, however, and suggest that secular resonance has mixed the Ananke and Pasiphae groups: three of the moons of the former family (Harpalyke, Praxidike and Iocaste) display similar grey colours (average colour indices: B−V = 0.77 and V−R = 0.42) while Ananke itself is on the boundary between grey and light red.^[7]

This diagram compares the orbital elements and relative sizes of the core members of the Ananke group. The horizontal axis illustrates their average distance from Jupiter, the vertical axis their orbital inclination, and the circles their relative sizes.

This diagram offers a wider field of view than the previous one, showing other small satellites clustered near the core Ananke group. (Philophrosyne and Eurydome were thought to be Ananke group members when this diagram was produced; they turned out to be Pasiphae group members.)

Notes

1. Negative period is indicative of retrograde motion.
2. 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 Gm in semi-major axis in 2 years, 0.5 in eccentricity in 12 years, and as much as 5° in inclination 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.

References

1. Jewitt, David C.; Sheppard, Scott S.; Porco, Carolyn (2004). Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (eds.). Jupiter. The planet, satellites, and magnetosphere (PDF). Jupiter's outer satellites and Trojans. Cambridge planetary science. Vol. 1. Cambridge, UK: Cambridge University Press. pp. 263–280. ISBN 0-521-81808-7. Archived from the original (PDF) on 2007-06-14.
2. Nesvorný, David; Beaugé, Cristian; Dones, Luke (2004). "Collisional Origin of Families of Irregular Satellites". The Astronomical Journal. 127 (3): 1768–1783. Bibcode:2004AJ....127.1768N. doi:10.1086/382099. S2CID 27293848 – via IOP Publishing.
3. "Moons of Jupiter". Earth & Planets Laboratory. Carnegie Institution for Science. 25 January 2024.
4. "Planetary Satellite Mean Elements". Jet Propulsion Laboratory. California Institute of Technology. 25 January 2024.
5. Nesvorný, David; Alvarellos, Jose L. A.; Dones, Luke; Levison, Harold F. (July 2003). "Orbital and Collisional Evolution of the Irregular Satellites" (PDF). The Astronomical Journal. 126 (1): 398–429. Bibcode:2003AJ....126..398N. doi:10.1086/375461. S2CID 8502734.
6. Sheppard, Scott S.; Jewitt, David C. (May 5, 2003). "An abundant population of small irregular satellites around Jupiter" (PDF). Nature. 423 (6937): 261–263. Bibcode:2003Natur.423..261S. doi:10.1038/nature01584. PMID 12748634. S2CID 4424447. Archived from the original (PDF) on August 13, 2006.
7. Grav, Tommy; Holman, Matthew J.; Gladman, Brett; Aksnes, Kaare (2003-01-02). "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 7793999.

External links