Planetary ring

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The moons Prometheus and Pandora shepherd the F ring of Saturn.

A planetary ring is a ring of cosmic dust and other small particles orbiting around a planet in a flat disc-shaped region. The most notable planetary rings known in the Solar System are those around Saturn, but the other three gas giants of the Solar System (Jupiter, Uranus and Neptune) also possess ring systems of their own.

On 26 March 2014, the discovery of rings around the centaur Chariklo by observing a stellar occultation was reported.[1][2][3] Pluto is not known to have any ring systems, though the New Horizons probe might find a ring system when it visits in 2015.[4]

Reports in March 2008[5][6][7] have suggested that the Saturnian moon Rhea may have its own tenuous ring system, which would make it the only moon known to possess a ring system. A later study published in 2010 revealed that imaging of Rhea from the Cassini mission was inconsistent with the predicted properties of the rings, suggesting that some other mechanism is responsible for the magnetic effects that had led to the ring hypothesis.[8]

Overview[edit]

The ring swirling around Saturn consists of chunks of ice and dust. The little dark spot on Saturn is the shadow from Saturn's moon Enceladus.

There are three ways that thicker planetary rings (the rings around planets) have been proposed to have formed: from material of the protoplanetary disk that was within the Roche limit of the planet and thus could not coalesce to form moons; from the debris of a moon that was disrupted by a large impact; or from the debris of a moon that was disrupted by tidal stresses when it passed within the planet's Roche limit. Most rings were thought to be unstable and to dissipate over the course of tens or hundreds of millions of years, but it now appears that Saturn's rings might be quite old, dating to the early days of the Solar System.[9]

Fainter planetary rings can form as a result of meteoroid impacts with moons orbiting around the planet or, in case of Saturn's E-ring, the ejecta of cryovolcanic material.[10][11]

The composition of ring particles varies; they may be silicate or icy dust. Larger rocks and boulders may also be present, and in 2007 tidal effects from eight 'moonlets' only a few hundred meters across were detected within Saturn's rings.

Sometimes rings will have "shepherd" moons, small moons that orbit near the outer edges of rings or within gaps in the rings. The gravity of shepherd moons serves to maintain a sharply defined edge to the ring; material that drifts closer to the shepherd moon's orbit is either deflected back into the body of the ring, ejected from the system, or accreted onto the moon itself.

Several of Jupiter's small innermost moons, namely Metis and Adrastea, are within Jupiter's ring system and are also within Jupiter's Roche limit.[12] It is possible that these rings are composed of material that is being pulled off these two bodies by Jupiter's tidal forces, possibly facilitated by impacts of ring material on their surfaces.

Uranus's ε ring also has two shepherd satellites, Cordelia and Ophelia, acting as inner and outer shepherds respectively.[13] Both moons are well within Uranus' synchronous orbit radius, and their orbits are therefore slowly decaying due to tidal deceleration.[14]

Neptune's rings are very unusual in that they first appeared to be composed of incomplete arcs in Earth-based observations, but Voyager 2's images showed them to be complete rings with bright clumps.[15] It is thought[16] that the gravitational influence of the shepherd moon Galatea and possibly other as-yet undiscovered shepherd moons are responsible for this clumpiness.

Pluto is not known to have any ring systems. However, some astronomers think that the New Horizons probe might find a ring system when it visits in 2015.[4]

It is also predicted that Phobos, a moon of Mars, will break up and form into a planetary ring in about 50 million years due to its low orbit.[17][18]

One minor planet is known to have rings, 10199 Chariklo. It has two rings, perhaps due to a collision that caused a chain of debris to orbit it. The rings came to light when astronomers watched Chariklo passing in front of the star UCAC4 248-108672 on June 3, 2013 from seven locations in South America. While watching, they saw two dips in the star’s apparent brightness just before and after the occultation. because this event was observed at multiple locations, the conclusion that the dip in brightness was in fact due to rings orbiting the asteroid is unanimously the leading theory. The observations revealed what is likely a 12.4-mile (20-kilometer)-wide ring system that is about 1,000 times closer the Moon is to Earth. In addition, astronomers suspect there could be a moon lying amidst the asteroid's ring debris. If these rings are the leftovers of a collision as astronomers suspect, this would give fodder to the idea that moons (such as the Moon) come to be from collisions of smaller bits of material. Chariklo's rings have not been officially named, but the discoverers have nicknamed them Oiapoque and Chuí, after two rivers near the northern and southern ends of Brazil.[19]

Visual comparison[edit]

A Galileo image of Jupiter's main ring.
A Cassini mosaic of Saturn's rings.
A Voyager 2 image of Uranus' rings.
A pair of Voyager 2 images of Neptune's rings.

Notes[edit]

  1. ^ "First Ring System Around Asteroid" (Press release). European Southern Observatory. 26 March 2014. Retrieved 2014-03-26. 
  2. ^ Gibney, E. (2014-03-26). "Asteroids can have rings too". Nature. doi:10.1038/nature.2014.14937.  edit
  3. ^ Braga-Ribas, F.; Sicardy, B.; Ortiz, J. L.; Snodgrass, C.; Roques, F.; Vieira-Martins, R.; Camargo, J. I. B.; Assafin, M.; Duffard, R.; Jehin, E.; Pollock, J.; Leiva, R.; Emilio, M.; Machado, D. I.; Colazo, C.; Lellouch, E.; Skottfelt, J.; Gillon, M.; Ligier, N.; Maquet, L.; Benedetti-Rossi, G.; Gomes, A. R.; Kervella, P.; Monteiro, H.; Sfair, R.; Moutamid, M. E.; Tancredi, G.; Spagnotto, J.; Maury, A. et al. (2014-03-26). "A ring system detected around the Centaur (10199) Chariklo". Nature 508 (7494): 72–75. doi:10.1038/nature13155. PMID 24670644.  edit
  4. ^ a b Steffl, Andrew J.; S. Alan Stern (2007). "First Constraints on Rings in the Pluto System". The Astronomical Journal 133 (4): 1485–1489. arXiv:astro-ph/0608036. Bibcode:2007AJ....133.1485S. doi:10.1086/511770. 
  5. ^ http://www.nasa.gov/mission_pages/cassini/media/rhea20080306.html NASA – Saturn's Moon Rhea Also May Have Rings
  6. ^ Jones, G. H.; et al. (2008-03-07). "The Dust Halo of Saturn's Largest Icy Moon, Rhea". Science (AAAS) 319 (5868): 1380–1384. Bibcode:2008Sci...319.1380J. doi:10.1126/science.1151524. PMID 18323452. 
  7. ^ Lakdawalla, E. (2008-03-06). "A Ringed Moon of Saturn? Cassini Discovers Possible Rings at Rhea". The Planetary Society web site. Planetary Society. Retrieved 2008-03-09. 
  8. ^ Tiscareno, Matthew S.; Burns, Joseph A.; Cuzzi, Jeffrey N.; Hedman, Matthew M. (2010). "Cassini imaging search rules out rings around Rhea". Geophysical Research Letters 37 (14): L14205. arXiv:1008.1764. Bibcode:2010GeoRL..3714205T. doi:10.1029/2010GL043663. 
  9. ^ "Saturn's Rings May Be Old Timers". NASA (News Release 2007-149). December 12, 2007. Retrieved 2008-04-11. 
  10. ^ Spahn, F. et al. (2006-03-10). "Cassini Dust Measurements at Enceladus and Implications for the Origin of the E Ring". Science (AAAS) 311 (5766): 1416–8. Bibcode:2006Sci...311.1416S. doi:10.1126/science.1121375. PMID 16527969. Retrieved 2008-09-13. 
  11. ^ Porco, C. C.; Helfenstein, P.; Thomas, P. C.; Ingersoll, A. P.; Wisdom, J.; West, R.; Neukum, G.; Denk, T.; Wagner, R. (10 March 2006). "Cassini Observes the Active South Pole of Enceladus". Science 311 (5766): 1393–1401. Bibcode:2006Sci...311.1393P. doi:10.1126/science.1123013. PMID 16527964.  edit
  12. ^ Gunter Faure, Teresa M. Mensing (2007). Introduction to Planetary Science: The Geological Perspective. Springer. ISBN 978-1-4020-5233-0. 
  13. ^ Esposito, L. W. (2002). "Planetary rings". Reports on Progress in Physics 65 (12): 1741–1783. Bibcode:2002RPPh...65.1741E. doi:10.1088/0034-4885/65/12/201. 
  14. ^ Karkoschka, Erich (2001). "Voyager's Eleventh Discovery of a Satellite of Uranus and Photometry and the First Size Measurements of Nine Satellites". Icarus 151 (1): 69–77. Bibcode:2001Icar..151...69K. doi:10.1006/icar.2001.6597.  edit
  15. ^ Miner, Ellis D., Wessen, Randii R., Cuzzi, Jeffrey N. (2007). "Present knowledge of the Neptune ring system". Planetary Ring System. Springer Praxis Books. ISBN 978-0-387-34177-4. 
  16. ^ Salo, Heikki; Hanninen, Jyrki (1998). "Neptune's Partial Rings: Action of Galatea on Self-Gravitating Arc Particles". Science 282 (5391): 1102–1104. Bibcode:1998Sci...282.1102S. doi:10.1126/science.282.5391.1102. PMID 9804544. 
  17. ^ Holsapple, K. A. (December 2001). "Equilibrium Configurations of Solid Cohesionless Bodies". Icarus 154 (2): 432–448. Bibcode:2001Icar..154..432H. doi:10.1006/icar.2001.6683. 
  18. ^ Gürtler, J. & Dorschner, J: "Das Sonnensystem", Barth (1993), ISBN 3-335-00281-4
  19. ^ "Surprise! Asteroid Hosts A Two-Ring Circus Above Its Surface". Universe Today. March 2014. 

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