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2014 UE228
2014 UE228 is a trans-Neptunian object from the outermost region of the Solar System. The object is in a rare 3:8 resonance with Neptune and measures approximately 93 kilometers (58 miles) in diameter. It was first observed on 22 October 2014, by astronomers with the Outer Solar System Origins Survey at the Mauna Kea Observatories, Hawaii, and was provisionally designated 2014 UE228. As of 2021[update], it has not been numbered.[2] Orbit and classification2014 UE228 orbits the Sun at a distance of 34.7–81.6 AU once every 443 years and 5 months (161,970 days; semi-major axis of 58.15 AU). Its orbit has an eccentricity of 0.40 and an inclination of 9° with respect to the ecliptic.[3] The body's observation arc begins at Mauna Kea on 9 August 2013, more than a year prior to its official discovery observation on 22 October 2014.[1][2] As of 2021[update], the object is about 37.8 AU from the Sun, with an apparent magnitude of 24.44,[7] and will come to perihelion in 2044.[3][8] 2014 UE228 is a resonant trans-Neptunian object that stays in a rare 3:8 mean-motion orbital resonance with Neptune, orbiting exactly three times the Sun for every 8 orbits Neptune does.[5] There are currently two other objects known to have the same resonant type: (82075) 2000 YW134 and (542258) 2013 AP183.[4][9] Long-term numerical integrations of the object's orbit by the Deep Ecliptic Survey shows a minimum perihelion distance of 34 AU. The classification is deemed secure.[5] Numbering and namingThis minor planet has neither been numbered nor named.[2] According to the established naming conventions, it will be given a mythological name associated with the underworld.[10] Physical characteristicsBased on a generic magnitude-to-diameter conversion, 2014 UE228 measures approximately 93 kilometers (58 miles) in diameter, for an assumed albedo of 0.9 and an absolute magnitude of 8.4.[4][6] As of 2021[update], no rotational lightcurve for this object has been obtained from photometric observations. The body's rotation period and pole as well as its albedo and surface composition remain unknown.[3] References
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