δScuti型变星BDS 1269 A的多重脉动频率激发  

Multiple Frequencies Pulsation of the δ Scuti Variable BDS 1269 A

作　　者：李治平[1] 蒋世仰[1] 

机构地区：[1]中国科学院北京天文台,北京100080

出　　处：《天体物理学报》1993年第3期233-244,共12页

基　　金：国家自然科学基金

摘　　要：以同一参考系归化Percy及Rucinski在1976年10月9日至11月6日获得的BDS1269A的光电测光数据后,利用多重周期分析方法进行周期分析,在周期初值的选取中尽可能穷尽所有可能的组合,最后根据最小残差获得最佳组合.我们认为BDS 1269 A的最佳频率解为:f_1=6.22999周每天,f_2=6.50840周每天,f_3=11.77324周每天,f_4=9.7136周每天,f_5=11.33694周每天.反证实验证明这组频率是充分的.基于以上频率解,一个非径向脉动目转分裂模型得以建立,其预言的自转速度。v_6=30km s^(-1)与BDS 1269A是一颗低速自转恒星的观测结果相吻合. 1987年10月16日至24日,我们取得了BDS1269 A的459个新的V波段光电观测点.上述频率解拟合此数据结果很好,拟合残差与观测误差一致.频率解得到了一次验证.A multi-period analysis has been conducted on the data set of BDS 1269 A made up of the observations obtained by Percy and Rucihski during October 9 to November 6, 1976. In our period analysis, many possible frequencies, which include all frequencies suspected, are selected to constitute the initial frequency estimates. By fitting various combinations of the initial frequencies to the data set, the best one can be determined, which has a minimum number of different frequencies with the lowest residuals. The best fitting frequency solution includes f1=6.22999 cycle d-t, f2 = 6.50840 cycle d-1, f3 = 11.77324 cycle d-1, f4= 9.71369 cycle d-1 and f3= 11.33694 cycled-1. The numeric experiment justifies this five-frequency solution. Based on this solution, a reasonable non-radial rotational splitting pulsation mode is identified, and a rotational velocity v3 = 30 km s-1 is predicted, which tends to agree with the fact that BDS 1269 A is a slowly rotational star.A total of 459 new measurements of four nights during 1987 October 16 to 24 were taken by authors with a Johnson V filter. The fitting with the five-frequency solution to the new data is very good with a residual which is near the uncertainty of the observation.

关 键 词：δScuti型 变星 周期分析 脉动频率 

分 类 号：P145.2[天文地球—天体物理]