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(505448) 2013 SA100
(505448) 2013 SA100, provisional designation 2013 SA100 and also known as o3l79,[2] is a trans-Neptunian object from the classical Kuiper belt in the outermost region of the Solar System. It was discovered on 5 August 2013, by astronomer with the Outer Solar System Origins Survey at the Mauna Kea Observatories, Hawaii, in the United States.[1] The classical Kuiper belt object belongs to the hot population and is a weak dwarf planet candidate, approximately 260 kilometers (160 miles) in diameter. Orbit and classificationIt orbits the Sun at a distance of 38.6–53.8 AU once every 314 years and 1 month (114,732 days; semi-major axis of 46.21 AU). Its orbit has an eccentricity of 0.16 and an inclination of 8° with respect to the ecliptic.[3] The body's observation arc begins with its official discovery observation at Mauna Kea Observatories in August 2013.[1] As a cubewano, also known as classical Kuiper belt object,[4] 2013 SA100 is located in between the resonant plutino and twotino populations and has a low-eccentricity orbit. With an inclination above 8°, it belongs to the "stirred" hot population rather than to the cold population with lower inclinations.[2] Numbering and namingThis minor planet was numbered by the Minor Planet Center on 4 November 2017 and received the number 505448 in the minor planet catalog (M.P.C. 107067).[6] As of 2018, it has not been named.[1] Physical characteristicsAccording to the American astronomer Michael Brown, 2013 SA100 measures 255 kilometers in diameter based on an assumed albedo of 0.08.[5] On his website, Brown lists this object as a "possible" dwarf planet (200–400 km), which is the category with the lowest certainty in his 5-class taxonomic system.[5] Similarly, Johnston's archive estimates a diameter 267 kilometers using an albedo of 0.09.[4] Spectroscopic measurements by the OSSOS team at the Gemini Observatory and with the Subaru Telescope gave a g–r and r–z color index of 0.61 and 0.47, respectively.[2] As of 2018, no rotational lightcurve has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.[3][7] References
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