User:Nrco0e/Notes/Rings of Haumea

Animation of Haumea with its ring

The minor planet and centaur 10199 Chariklo, with a diameter of about 250 kilometres (160 mi), is the smallest celestial object with confirmed rings and the fifth ringed celestial object discovered in the Solar System, after the gas giants and ice giants. Orbiting Chariklo is a bright ring system consisting of two narrow and dense bands, 6–7 km (4 mi) and 2–4 km (2 mi) wide, separated by a gap of 9 kilometres (6 mi). The rings orbit at distances of about 400 kilometres (250 mi) from the centre of Chariklo, a thousandth the distance between Earth and the Moon. The discovery was made by a team of astronomers using ten telescopes at various locations in Argentina, Brazil, and Chile in South America during observation of a stellar occultation on 3 June 2013, and was announced on 26 March 2014.

The existence of a ring system around a minor planet was unexpected because it had been thought that rings could only be stable around much more massive bodies. Ring systems around minor bodies had not previously been discovered despite the search for them through direct imaging and stellar occultation techniques. Chariklo's rings should disperse over a period of at most a few million years, so either they are very young, or they are actively contained by shepherd moons with a mass comparable to that of the rings. The team nicknamed the rings Oiapoque (the inner, more substantial ring) and Chuí (the outer ring), after the two rivers that form the northern and southern coastal borders of Brazil. A request for formal names will be submitted to the IAU at a later date.

Discovery

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Occultation

Origin

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Formation of Haumea and its collisional history

Properties

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Orientation, composition, brightness, opacity

The orientation of the rings is consistent with an edge-on view from Earth in 2008, explaining the observed dimming of Chariklo between 1997 and 2008 by a factor of 1.75, as well as the gradual disappearance of water ice and other materials from its spectrum as the observed surface area of the rings decreased. Also consistent with this edge-on orientation is that since 2008, the Chariklo system has increased in brightness by a factor of 1.5 again, and the infrared water-ice spectral features have reappeared. This suggests that the rings are composed at least partially of water ice. An icy ring composition is also consistent with the expected density of a disrupted body within Chariklo's Roche limit.

Rings of Chariklo
Name Nickname Orbital radius (km) Width (km) Optical depth Surface density (g/cm2) Size-equivalent mass Gap between rings (km) Radial separation (km)
2013C1R Oiapoque 390.6±3.3 6.16±0.11 to 7.17±0.14 0.449±0.009 to 0.317±0.008 30–100 icy body ~1 km in diameter 8.7±0.4 14.2±0.2
2013C2R Chuí 404.8±3.3 3.4+1.3
−2.0
to 3.6+1.1
−1.4
0.05+0.06
−0.01
to 0.07+0.05
−0.03
? icy body ~0.5 km in diameter

Dynamics

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Orbit, resonances, eccentricity and inclination, precession and influence by Haumea's moons

Telescopes and observatories

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Haumea resources

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The dynamics of rings around Centaurs and Trans-Neptunian objects, The Trans-Neptunian Solar System by Sicardy et al. (2020)

Discovery

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Properties

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Orientation

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Dynamics

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Precession

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External effects

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Origin

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