对测定望远镜视场畸变的星对法的改进  

IMPROVEMENT TO THE STAR PAIR METHOD FOR DETERMINATION OF TELESCOPE OBJECTIVE DISTORTION

作　　者：鲁春林[1] 李东明[1] 

机构地区：[1]中国科学院紫金山天文台

出　　处：《天文学报》1990年第2期153-157,共5页Acta Astronomica Sinica

摘　　要：本文介绍改进的测定望远镜视场畸变的星对法.这种方法克服了传统星对法的缺点.理论上是严格的,每张底片可以用很多星对来测定畸变系数.文中还给出了这种方法用于紫金山天文台双简照相望远镜的初步结果.An improved star pair method for determination of telescope objective distortion is introduced. In this method, the effect of central projection is removed with equation (4), where Lo is the linear distance between the two stars in the pair when the tangent point is located at the center of the star pair, the meanings of d, r_1 and r_2 are illustrated in Fig.1. If the foot of perpendicular of tangent point on the line joining the two star is between them, the '±' takes '-', otherwise '+'. Then the distortion cofficient v can be deermined with equation (8), where subscript 'o' denates the exposure near the plate cenper, '1' the exposure farther from the center. the meanings of symbols can be seen in Fig.1. This method is theoretically strict. it eliminated the defects of the classical star pair method. With this method, a number of star pairs on a plate can be used in the determination of distortion. The primary results of application of the method to the twin astrograph at Purple mountain Observatory are presented.

关 键 词：望远镜 视场 畸变 星对法 象差 

分 类 号：P123[天文地球—天体测量]