Carme group

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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 22.9 and 24.1 Gm, their orbital inclinations between 164.9° and 165.5°, and their orbital eccentricities between 0.23 and 0.27 (with one exception).

This diagram illustrates the largest irregular satellites of Jupiter. The location of the Carme group is illustrated by Carme's presence in the lower middle. 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. TheIrregulars JUPITER GROUPS.svg
This diagram illustrates the largest irregular satellites of Jupiter. The location of the Carme group is illustrated by Carme's presence in the lower middle. 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.


The core members include (negative period indicates retrograde orbit): [1] [2]

This diagram compares the orbital elements and relative sizes of the core members of the Carme group. The horizontal axis illustrates their average distance from Jupiter, the vertical axis their orbital inclination, and the circles their relative sizes. TheIrregulars JUPITER Carme CORE.svg
This diagram compares the orbital elements and relative sizes of the core members of the Carme group. The horizontal axis illustrates their average distance from Jupiter, the vertical axis their orbital inclination, and the circles their relative sizes.
NameDiameter
(km)		Period
(days)		Notes
Carme 46.7−693.17 [3] largest member and group prototype
Taygete 5−691.62 [4]
Eukelade [5] 4−693.02 [3]
Eirene [5] 3−743.88 [6]
Chaldene 4−759.88 [7]
Isonoe 4−688.61 [7]
Kalyke 6.9−766.61 [7] substantially redder than the others
Erinome 3−682.80 [3]
Aitne 3−712.04 [7]
Kale 2−736.55 [3]
Pasithee 2−711.12 [3]
S/2003 J 9 (probably) [5] 1−767.60 [8]

The International Astronomical Union (IAU) reserves names ending in -e for all retrograde moons.

Origin

The very low dispersion of the mean 1 orbital elements among the core members (the group is separated by less than 700,000 km in semi major axis and less than 0.7° 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). [9] 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. [10]

Further support to the single body origin comes from the known colours: all2 the satellites appear light red, with colour indices B-V= 0.76 and V-R= 0.47 [11] and infrared spectra, similar to D-type asteroids. [12] These data are consistent with a progenitor from the Hilda family or a Jupiter Trojan.

1 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 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.
2With the exception of Kalyke, substantially redder.

This diagram shows the Ananke group on the same scale as the other diagram, illustrating its wide dispersion in comparison with the compact Carme group (see related diagram). TheIrregulars JUPITER Ananke.svg
This diagram shows the Ananke group on the same scale as the other diagram, illustrating its wide dispersion in comparison with the compact Carme group (see related diagram).
This diagram shows the compactness of the Carme group. TheIrregulars JUPITER Carme.svg
This diagram shows the compactness of the Carme group.

Related Research Articles

<span class="mw-page-title-main">Carme (moon)</span> Moon of Jupiter

Carme is a retrograde irregular satellite of Jupiter. It was discovered by Seth Barnes Nicholson at Mount Wilson Observatory in California in July 1938. It is named after the mythological Carme, mother by Zeus of Britomartis, a Cretan goddess.

<span class="mw-page-title-main">Lysithea (moon)</span> Outer moon of Jupiter

Lysithea is a prograde irregular satellite of Jupiter. It was discovered by Seth Barnes Nicholson in 1938 at Mount Wilson Observatory and is named after the mythological Lysithea, daughter of Oceanus and one of Zeus' lovers.

<span class="mw-page-title-main">Caliban (moon)</span> Moon of Uranus

Caliban is the second-largest retrograde irregular satellite of Uranus. It was discovered on 6 September 1997 by Brett J. Gladman, Philip D. Nicholson, Joseph A. Burns, and John J. Kavelaars using the 200-inch Hale telescope together with Sycorax and given the temporary designation S/1997 U 1.

<span class="mw-page-title-main">Ananke (moon)</span> Moon of Jupiter

Ananke is a retrograde irregular moon of Jupiter. It was discovered by Seth Barnes Nicholson at Mount Wilson Observatory in 1951 and is named after the Greek mythological Ananke, the personification of necessity, and the mother of the Moirai (Fates) by Zeus. The adjectival form of the name is Anankean.

<span class="mw-page-title-main">Pasiphae (moon)</span> Moon of Jupiter

Pasiphae, formerly spelled Pasiphaë, is a retrograde irregular satellite of Jupiter. It was discovered in 1908 by Philibert Jacques Melotte and later named after the mythological Pasiphaë, wife of Minos and mother of the Minotaur from Greek legend.

<span class="mw-page-title-main">Sinope (moon)</span> Moon of Jupiter

Sinope is a retrograde irregular satellite of Jupiter discovered by Seth Barnes Nicholson at Lick Observatory in 1914, and is named after Sinope of Greek mythology.

<span class="mw-page-title-main">Themisto (moon)</span> Outer moon of Jupiter

Themisto, also known as Jupiter XVIII, is a small prograde irregular satellite of Jupiter. It was discovered in 1975, subsequently lost, and rediscovered in 2000.

<span class="mw-page-title-main">Kale (moon)</span>

Kale, also known as Jupiter XXXVII, is a retrograde irregular satellite of Jupiter. It was discovered in 2001 by astronomers Scott S. Sheppard, D. Jewitt, and J. Kleyna, and was originally designated as S/2001 J 8.

<span class="mw-page-title-main">Sycorax (moon)</span> Moon of Uranus

Sycorax is the largest irregular satellite of Uranus. Sycorax was discovered on 6 September 1997 by Brett J. Gladman, Philip D. Nicholson, Joseph A. Burns, and John J. Kavelaars using the 200-inch Hale telescope, together with Caliban, and given the temporary designation S/1997 U 2.

<span class="mw-page-title-main">Moons of Jupiter</span> Natural satellites of the planet Jupiter

There are 95 moons of Jupiter with confirmed orbits as of 23 October 2023. This number does not include a number of meter-sized moonlets thought to be shed from the inner moons, nor hundreds of possible kilometer-sized outer irregular moons that were only briefly captured by telescopes. All together, Jupiter's moons form a satellite system called the Jovian system. The most massive of the moons are the four Galilean moons: Io, Europa, Ganymede, and Callisto, which were independently discovered in 1610 by Galileo Galilei and Simon Marius and were the first objects found to orbit a body that was neither Earth nor the Sun. Much more recently, beginning in 1892, dozens of far smaller Jovian moons have been detected and have received the names of lovers or daughters of the Roman god Jupiter or his Greek equivalent Zeus. The Galilean moons are by far the largest and most massive objects to orbit Jupiter, with the remaining 91 known moons and the rings together composing just 0.003% of the total orbiting mass.

<span class="mw-page-title-main">Harpalyke (moon)</span> Retrograde irregular satellite of Jupiter

Harpalyke, also known as Jupiter XXII, is a retrograde irregular satellite of Jupiter. It was discovered by a team of astronomers from the University of Hawaii led by Scott S. Sheppard in 2000, and given the temporary designation S/2000 J 5. In August 2003, the moon was named after Harpalyke, the incestuous daughter of Clymenus, who in some accounts was also a lover of Zeus (Jupiter).

<span class="mw-page-title-main">Praxidike (moon)</span> Moon of Jupiter

Praxidike, also known as Jupiter XXVII, is a retrograde irregular satellite of Jupiter. It was discovered by a team of astronomers from the University of Hawaii led by Scott S. Sheppard in 2000, and given the temporary designation S/2000 J 7.

<span class="mw-page-title-main">Iocaste (moon)</span> Retrograde irregular satellite of Jupiter

Iocaste, also known as Jupiter XXIV, is a retrograde irregular satellite of Jupiter. It was discovered by a team of astronomers from the University of Hawaii including: David C. Jewitt, Yanga R. Fernandez, and Eugene Magnier led by Scott S. Sheppard in 2000, and given the temporary designation S/2000 J 3.

<span class="mw-page-title-main">Taygete (moon)</span> Moon of Jupiter

Taygete, also known as Jupiter XX, is a retrograde irregular satellite of Jupiter. It was discovered by a team of astronomers from the University of Hawaii led by Scott S. Sheppard, in 2000, and given the temporary designation S/2000 J 9.

<span class="mw-page-title-main">Kalyke</span> Moon of Jupiter

Kalyke, also known as Jupiter XXIII, is a retrograde irregular satellite of Jupiter. It was discovered by a team of astronomers from the University of Hawaii led by Scott S. Sheppard in 2000, and given the temporary designation S/2000 J 2.

<span class="mw-page-title-main">Neso (moon)</span> Outermost moon of Neptune

Neso, also known as Neptune XIII, is the outermost known natural satellite of Neptune. It is a retrograde irregular moon discovered by Matthew J. Holman, Brett J. Gladman, et al. on 14 August 2002, though it went unnoticed until 2003. Neso orbits Neptune at a distance of more than 48 Gm, making it the most distant known moon of any planet. At apocenter, the satellite is more than 72 Gm from Neptune. This distance exceeds Mercury's aphelion, which is approximately 70 Gm from the Sun.

<span class="mw-page-title-main">Himalia group</span> Satellites of Jupiter

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

<span class="mw-page-title-main">Ananke group</span> Group of retrograde irregular satellites of Jupiter

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.

<span class="mw-page-title-main">Pasiphae group</span>

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

<span class="mw-page-title-main">Irregular moon</span> Captured satellite following an irregular orbit

In astronomy, an irregular moon, irregular satellite or irregular natural satellite is a natural satellite following a distant, inclined, and often eccentric and retrograde orbit. They have been captured by their parent planet, unlike regular satellites, which formed in orbit around them. Irregular moons have a stable orbit, unlike temporary satellites which often have similarly irregular orbits but will eventually depart. The term does not refer to shape; Triton for example, is a round moon, but is considered irregular due to its orbit.

References

  1. ↑ 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 Full text(pdf). Archived June 14, 2007, at the Wayback Machine
  2. ↑ David Nesvorný, Cristian Beaugé, and Luke Dones Collisional Origin of Families of Irregular Satellites, The Astronomical Journal, 127 (2004), pp. 1768–1783 Full text.
  3. 1 2 3 4 5 "M.P.C. 127087-127088" (PDF). Minor Planet Circular. Minor Planet Center. 17 November 2020.
  4. ↑ "M.P.C. 110499" (PDF). Minor Planet Circular. Minor Planet Center. 29 May 2018.
  5. 1 2 3 Listed by Nesvorný 2004 as a possible member, not listed by Sheppard 2004; the orbital elements confirmed by Jacobson 2004
  6. ↑ "M.P.C. 115250" (PDF). Minor Planet Circular. Minor Planet Center. 9 June 2017.
  7. 1 2 3 4 "M.P.C. 115890-115891" (PDF). Minor Planet Circular. Minor Planet Center. 27 August 2019.
  8. ↑ "MPEC 2020-V19 : S/2003 J 9". Minor Planet Electronic Circular. Minor Planet Center. 5 November 2020. Retrieved 5 November 2020.
  9. ↑ 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. (pdf) Archived 15 April 2020 at the Wayback Machine
  10. ↑ 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.
  11. ↑ Grav, Tommy; Holman, Matthew J.; Gladman, Brett J.; Aksnes, Kaare Photometric survey of the irregular satellites, Icarus, 166,(2003), pp. 33–45. Preprint
  12. ↑ Tommy Grav and Matthew J. Holman Near-Infrared Photometry of the Irregular Satellites of Jupiter and Saturn,The Astrophysical Journal, 605, (2004), pp. L141–L144 Preprint
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