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HD 106906 b
HD 106906 b is a directly imaged planetary-mass companion〔 and candidate exoplanet orbiting the star , in the constellation Crux at about 300 light-years from Earth.〔 It is estimated to be about eleven times the mass of Jupiter and is located about 650 AU, or nearly 97 billion kilometres (60 billion miles), away from its host star.〔 is unique to science; while its mass estimate is nominally consistent with identifying it as an exoplanet, it appears at a much wider separation from its parent star than thought possible for in-situ formation from a protoplanetary disk.
==Description==
is the only known companion orbiting , an F-type pre-main-sequence star with about 1.5 times the Sun's mass and 6 times its luminosity.〔 Based on the star's luminosity and temperature, the system is estimated to be about 13 million years old. The system is a likely member of the Scorpius–Centaurus Association. The star is surrounded by a luminous, massive debris disk at a much smaller separation than .〔 Based on its near-infrared spectral-energy distribution, its age, and relevant evolutionary models, is estimated to be eleven times the mass of Jupiter, with a surface temperature of .〔 The high surface temperature, a relic of its recent formation, gives it a luminosity of about 0.02% of the Sun's.〔 While its mass and temperature are similar to other planetary-mass companions/exoplanets like or , its projected separation from the star is much larger, about 650 AU,〔 giving it one of the widest orbits of any currently known planetary-mass companions.〔
The measurements obtained thus far are not adequate to evaluate its orbital properties. If its eccentricity is large enough, it might approach the outer edge of the primary's debris disk closely enough to interact with it at periastron. In such a case, the outer extent of the debris disk would be truncated at the inner edge of Hill sphere at periastron, or at its periastron minus 15 AU for a limit around 120 AU (see below).〔
The discovery team evaluated the possibility that is not gravitationally bound to , but is seen close to it along our line of sight and moving in the same direction by chance. The odds of such a coincidence were found to be less than 0.01%.〔
抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』
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