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A Star transit is the passage of a star through the eyepiece of a telescope. The precise observation of star transits is the basis of many methods in Astronomy and in Geodesy. The measurements can be done in different ways: # visually (mostly up to 1990): accuracy 0,1" to 2" (depending on the instrument); timing with digital clocks about 0,05-0,2 seconds # by CCD and other electro-optical sensors: as above, time often better # semi automatic instruments: Photography or "impersonal micrometer", ca. 2 times better than No.1 # by Scanning methods: Astrometry satellites like Hipparcos about 0,01". ==Literature== * Karl Ramsayer, 1969: ''Geodätische Astronomie'', Vol.2a of Handbuch der Vermessungskunde, 900 p., J.B.Metzler-Verlag Stuttgart. * Ivan I. Mueller, 1969: Spherical and Practical Astronomy as applied to Geodesy, 610 p., Fred.Ungar publ., USA * IAU Coll.48: ''Modern Astrometry'', Egermann, University Vienna. 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「star transit」の詳細全文を読む スポンサード リンク
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