Matches in DBpedia 2016-04 for { ?s ?p "(55636) 2002 TX300 is a bright Kuiper belt object in the outer Solar System estimated to be about 286 kilometres (178 mi) in diameter. It is a large member of the Haumea family that was discovered on October 15, 2002 by the Near-Earth Asteroid Tracking (NEAT) program.2002 TX300 is a classical Kuiper belt object with an absolute magnitude between that of 50000 Quaoar and 20000 Varuna. 2002 TX300 has the most eccentric and inclined orbit of the three.A variability of the visual brightness was also detected which could fit to 7.9 h or 15.8 h rotational period (the distinction between single or double-peaked curved could not be made with confidence). The changes in brightness are quite close to the error margin and could also be due to an irregular shape."@en }
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- (55636)_2002_TX300 abstract "(55636) 2002 TX300 is a bright Kuiper belt object in the outer Solar System estimated to be about 286 kilometres (178 mi) in diameter. It is a large member of the Haumea family that was discovered on October 15, 2002 by the Near-Earth Asteroid Tracking (NEAT) program.2002 TX300 is a classical Kuiper belt object with an absolute magnitude between that of 50000 Quaoar and 20000 Varuna. 2002 TX300 has the most eccentric and inclined orbit of the three.A variability of the visual brightness was also detected which could fit to 7.9 h or 15.8 h rotational period (the distinction between single or double-peaked curved could not be made with confidence). The changes in brightness are quite close to the error margin and could also be due to an irregular shape.".
- Q155535 abstract "(55636) 2002 TX300 is a bright Kuiper belt object in the outer Solar System estimated to be about 286 kilometres (178 mi) in diameter. It is a large member of the Haumea family that was discovered on October 15, 2002 by the Near-Earth Asteroid Tracking (NEAT) program.2002 TX300 is a classical Kuiper belt object with an absolute magnitude between that of 50000 Quaoar and 20000 Varuna. 2002 TX300 has the most eccentric and inclined orbit of the three.A variability of the visual brightness was also detected which could fit to 7.9 h or 15.8 h rotational period (the distinction between single or double-peaked curved could not be made with confidence). The changes in brightness are quite close to the error margin and could also be due to an irregular shape.".