Ananke (moon)

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Ananke
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Ananke photographed by the Haute-Provence Observatory in August 1998
Discovery[1]
Discovered bySeth B. Nicholson
Discovery siteMt. Wilson Observatory
Discovery date28 September 1951
Designations
Designation
Jupiter XII
Pronunciation/əˈnæŋkiː/[2]
Named after
Ἀνάγκη Anagkē
AdjectivesAnankean /ænəŋˈkiːən/[3]
Orbital characteristics[4]
Epoch 17 December 2020 (JD 2459200.5)
Observation arc69.05 yr (24,338 days)
Template:Cvt
Eccentricity0.1747248
–623.59 d
339.61045°
Template:Deg2DMS / day
Inclination148.67482° (to ecliptic)
86.44368°
135.63033°
Satellite ofJupiter
GroupAnanke group
Physical characteristics
29.1±0.6 km[5]
Mass1.68×1016 kg (calculated)
Mean density
1.30 g/cm3 (assumed)[6]
8.31±0.15 h[7]
Albedo0.038±0.006[5]
Spectral type
P[5]
18.9[8]
11.7[4]
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Ananke (/əˈnæŋki/), also known as Jupiter XII, is one of the larger retrograde irregular moons of Jupiter.

Discovery and naming

It was discovered by Seth Barnes Nicholson at Mount Wilson Observatory in 1951.[1]

It is named after the Greek mythological Ananke, the personification of necessity, and the mother of the Moirai (Fates) by Zeus. Ananke did not receive its present name[9] until 1975;[10] before then, it was simply known as Jupiter XII. It was sometimes called "Adrastea"[11] between 1955 and 1975 (Adrastea is now the name of another satellite of Jupiter).

Orbit

Ananke orbits Jupiter (on average 21,042,470 km) on a high-eccentricity (0.174) and high-inclination (149° to ecliptic) retrograde orbit. They are continuously changing due to solar and planetary perturbations.

Ananke gives its name to the Ananke group, a group of irregular retrograde moons orbiting Jupiter at a distance ranging between 19–22 million km, with inclinations between 144 and 156°, and eccentricities between 0.10 and 0.30.

Physical characteristics

Single-exposure image of Ananke by the Wide-field Infrared Survey Explorer (WISE) spacecraft in 2010

From infrared thermal measurements by the WISE spacecraft, Ananke's albedo is measured at 3.8%, corresponding to a diameter of 29.1 kilometres.[5]

In the visible spectrum, Ananke appears neutral to light-red (colour indices B-V=0.90 V-R=0.38).[12] The infrared spectrum is similar to P-type asteroids but with a possible indication of water.[13]

The rotation period was determined to be approximately 8 hours and 18.6 minutes with a peak amplitude of about ~0.4 magnitudes.[7] This was regarded by a later paper as uncertain due to the short observation periods.[14]

Origin

Ananke probably did not form near Jupiter but was captured by Jupiter later. Given these orbital elements and the physical characteristics known so far, Ananke is thought to be the largest remnant[15] of an original break-up, forming the Ananke group.[16][12]

See also

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References

  1. ^ a b Page Module:Citation/CS1/styles.css has no content.Nicholson, S. B. (1951). "An unidentified object near Jupiter, probably a new satellite". Publications of the Astronomical Society of the Pacific. 63 (375): 297–299. Bibcode:1951PASP...63..297N. doi:10.1086/126402.
  2. ^ Template:Dict.com
  3. ^ Yenne (1987) The Atlas of the Solar System.
  4. ^ a b Page Module:Citation/CS1/styles.css has no content."M.P.C. 127087" (PDF). Minor Planet Circular. Minor Planet Center. 17 November 2020.
  5. ^ a b c d Page Module:Citation/CS1/styles.css has no content.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.
  6. ^ Page Module:Citation/CS1/styles.css has no content.Chen, Zhenghan; Yang, Kun; Liu, Xiaodong (6 February 2024). "'Life' of dust originating from the irregular satellites of Jupiter". Monthly Notices of the Royal Astronomical Society. 527 (4): 11327–11337. arXiv:2402.03680. doi:10.1093/mnras/stad3829.
  7. ^ a b Page Module:Citation/CS1/styles.css has no content.Luu, Jane (September 1991). "CCD photometry and spectroscopy of the outer Jovian satellites". Astronomical Journal. 102: 1213–1225. Bibcode:1991AJ....102.1213L. doi:10.1086/115949. ISSN 0004-6256.
  8. ^ Page Module:Citation/CS1/styles.css has no content.Sheppard, Scott. "Scott S. Sheppard - Jupiter Moons". Department of Terrestrial Magnetism. Carnegie Institution for Science. Retrieved 26 November 2020.
  9. ^ Page Module:Citation/CS1/styles.css has no content.Nicholson, S.B. (April 1939). "The Satellites of Jupiter". Publications of the Astronomical Society of the Pacific. 51 (300): 85–94. Bibcode:1939PASP...51...85N. doi:10.1086/125010.
  10. ^ Page Module:Citation/CS1/styles.css has no content.Marsden, B. G. (7 October 1974). "Satellites of Jupiter". IAU Circular. 2846.
  11. ^ Page Module:Citation/CS1/styles.css has no content.Payne-Gaposchkin, Cecilia; Katherine Haramundanis (1970). Introduction to Astronomy. Englewood Cliffs, N.J.: Prentice-Hall. ISBN 0-13-478107-4.
  12. ^ a b Page Module:Citation/CS1/styles.css has no content.Grav, Tommy; Holman, M. J.; Gladman, B. J.; Aksnes, K. (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 7793999.
  13. ^ Page Module:Citation/CS1/styles.css has no content.Grav, Tommy; Holman, Matthew J. (2004). "Near-Infrared Photometry of the 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.
  14. ^ Page Module:Citation/CS1/styles.css has no content.Denk, Tilmann; Williams, David A.; Tosi, Federico; Bell III, James F.; Mottola, Stefano; de Pater, Imke; et al. (5 March 2026). "Io and the Minor Jovian Moons – Prospects for JUICE". Space Science Reviews. 222 (2) 27. Bibcode:2026SSRv..222...27D. doi:10.1007/s11214-025-01263-6.
  15. ^ Page Module:Citation/CS1/styles.css has no content.Sheppard, S.S.; Jewitt, D.C. (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 13 August 2006.
  16. ^ Page Module:Citation/CS1/styles.css has no content.Nesvorný, D.; Beaugé, C.; Dones, L. (2004). "Collisional Origin of Families of Irregular Satellites". The Astronomical Journal. 127 (3): 1768–1783. Bibcode:2004AJ....127.1768N. doi:10.1086/382099.

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