论文标题
SX PHE Star BL CAM的光度和光谱分析
Photometric and Spectroscopic Analysis of the SX Phe Star BL Cam
论文作者
论文摘要
在本文中，我们报告了由1.88 m望远镜在脉动星体BL CAM的Kottamia天文通观测到的1.88 m望远镜获得的光度和光谱观测。光曲线的傅立叶分析表明，基本模式具有两个谐波。 O-C方法用于建立周期更改。到目前为止，该分析在映射恒星在整个不稳定性条上的脉动幅度方面非常成功。通过使用Eddington和Plakidis（1929）的形式主义，我们发现了进化时期变化的重大结果和有力的迹象。总共报告了55个新的最大光定时。 （1/p）dp/dt的新值使用O-C图估算了所有新获得的最大光的时间与从文献中获取的时间相结合的新值，假设这些周期正在降低并平稳地变化。为了计算恒星的有效温度和表面重力，我们对其光谱进行了模型大气分析。计算恒星的物理参数，并将其与进化模型进行比较。
In the present paper, we report the photometric and spectroscopic observations obtained by the 1.88 m telescope at the Kottamia astronomical observatory of the pulsating star BL Cam. Fourier analysis of the light curves reveals that the fundamental mode has two harmonics. The O-C method is used to establish the period changes. So far, the analysis has been very successful in mapping the pulsation amplitude of the star across the instability strip. By using the formalism of Eddington and Plakidis (1929), we found significant results and strong indications of the evolutionary period change. A total of 55 new maximum light timings are reported. New values of (1/P) dP/dt are estimated using the O-C diagram based on all newly obtained times of maximum light combined with those taken from the literature, assuming the periods are decreasing and changing smoothly. To compute the effective temperature and surface gravity of the star, we performed model atmosphere analysis on its spectra. The physical parameters of the star are calculated and compared with the evolutionary models.
