A novel bright‐star identification algorithm is presented using the time series of vertical angle and horizontal angle velocity observed by the total station .The algorithm can distinguish planets from the starry background with automatically computing for the horizontal coordinates of the observed target . Based on the investigation of measurement errors , the matching thresholds and the effective matching strategy are given .Tests results with simul ated and actual measurements show that the success rate of identification can be up to 100% ,which is much higher than the existing algorithm .Then the identification algorithm is applied to the astronomical azimuth determination with the measurements of some bright stars and pl anets and the resulting precision and accuracy are 1 6.″and 2 0.″,respectively .Finally ,it is pointed that multi‐star observations can improve the accuracy of the astronomical orientation by effectively removing the impact of errors of station coordinates .The presented orientation method can be extended to cloudy or haze weather when only few visible bright stars can be observed .%基于全站仪对任意亮星的观测采样，提出了一种利用高度角序列和水平角速率进行联合匹配的任意亮星识别算法。通过引入天体地平坐标计算程序，算法可正确辨别行星和恒星。本文分析了任意亮星高度角和水平角速率的观测误差和计算误差，以此给出了匹配阈值条件的设定依据，并在此基础上制定了有效的匹配策略。仿真计算及实际观测试验均表明，该算法具有100％的识别成功率，远优于现有算法。将此算法应用于任意亮星天文定向，定向结果的内符合精度达到2″，外部检核精度达到16．″。采用多颗任意亮星进行定向，可有效减弱由测站位置误差引入的定向系统误差，提高绝对定向精度。本文提出的天文定向适用于多云及雾霾天气。
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