摘要
利用文[1]中权重5的大量高精度测光数据,用文[2]中的周期分析法,得出BWVul的主要脉动周期P_1=0.21010425d。另有变幅仅为前者十分之一的二倍频P_2=0.10052300d及四倍频P_4=0.05026096d。文[3]求出的变幅更小的P_3、P_5、P_6、P_7、P_8等倍频可信度很低。故多重周期不是引起P_1长期变化及限制脉动变幅的主因。
In this paper we use the high accurate observations published in paper [1] (with weight 5 only) and the method shown in paper [2] to analyse the periods of the beta Cep type variable BW Vul. We find that this star is mainly pulsating with a period P1 = 0.2010425 d. Although there exist other two resonant periods P2 = 0.100523d and P3= 0.0502609 d, their amplitudes are one magnitude smaller than that of the first one. So there is no another period colse to period P1. It seems that the long period of about 26.3 years found in the (O-C) curve of the maximum time is caused by light time effect of binary orbital movement instead <of beat pulsating periods. However, recent observations show that this long period variation may not be sinusoidal but tooth-shaped. That is to say it may be caused by structure abrupte variations of this star.
