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半人馬座Xi2
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半人马座Xi2 （ξ2 Cen, ξ2 Centauri）是在南天半人马座的三星系统[12]，这较宽的光学双星视星等为裸眼可见的+4.30等[2]，略比半人马座ξ1A型主序星暗[13]（+4.83等[14]），年周视差6.98mas，距离太阳大约470光年。在这样的距离，恒星会因为中间的星际尘埃造成消光，而使视星等减弱0.32等[15]
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This system was discovered to be a single-lined spectroscopic binary in 1910 by American astronomer Joseph Haines Moore.[16][17] The pair, component A, orbit each other with a period of 7.6497 days and an eccentricity of 0.35.[8] The primary is a B-type star with a stellar classification of B1.5 V[4] or B2 IV,[5] depending on the source. This indicates it may be a main sequence star or a more evolved subgiant star. It has about 8.1[4] times the mass of the Sun and radiates 1,702 times the solar luminosity from its outer atmosphere at an effective temperature of 20,790 K.[9] It is a hybrid pulsator and shows spacings in both g and p modes.[18]
A third star, component B, is a magnitude 9.38 F-type main sequence star with a classification of F7 V. It has 1.25[9] times the mass of the Sun and radiates 2.4[9] times the solar luminosity at an effective temperature of 6,194[9] K. It lies at an angular separation of 25.1 arc seconds from the inner pair.[3] They share a common proper motion, indicating they may be gravitationally bound with an orbital period of around 41,000 years.[19]
The system has a peculiar velocity of 16.2±4.2 km/s.[6] It belongs to the Scorpius–Centaurus association and appears to be a member of the Gould's Belt.[20]
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