Curious Variables Experiment (CURVE). Three Periodicities of BF Ara
Curious Variables Experiment (CURVE). Three Periodicities of BF Ara
复制标题
好奇变量实验（CURVE）。
DOI：
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发表时间：
2008
期刊：
影响因子：
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通讯作者：
A. Schwarzenberg
中科院分区：
文献类型：
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作者：
A. Olech;A. Rutkowski;A. Schwarzenberg
我们报告了矮新星 BF Ara 在连续 15 个静止夜晚的 CCD 光度测量。该区间的光变曲线以 0.8 星等左右的大幅度调制为主，由两个周期组成。较高振幅信号的特征是周期为 0.082159(4) 天，其以 dotP/Psh = 3.8(3)* 10^{-5} 的速率增加。较弱且稳定的信号周期为0.084176(21)天。了解 Kato 等人确定的 BF Ara 超级驼峰周期。 (2003) 且等于 0.08797(1) 天，第一个调制被解释为由标题吸积盘的逆行进动引起的静态负超级驼峰，而后一个调制被解释为双星的轨道周期。相应的周期超出和缺陷为 epsilon_+ = 4.51% +/- 0.03% 和 epsilon_- = -2.44% +/- 0.02%。因此，BF Ara 是另一颗间隙新星，质量比 q 约为 0.21。
We report CCD photometry of the dwarf nova BF Ara throughout fifteen consecutive nights in quiescence. Light curve in this interval is dominated by a large amplitude around 0.8 mag modulation consisting two periods. Higher amplitude signal is characterized by period of 0.082159(4) days, which was increasing at the rate of dotP/Psh = 3.8(3)* 10^{-5}. Weaker and stable signal has period of 0.084176(21) days. Knowing the superhump period of BF Ara determined by Kato et al. (2003) and equal to 0.08797(1) days, the first modulation is interpreted as quiescent negative superhump arising from retrograde precesion of titled accretion disk and the latter one as an orbital period of the binary. The respective period excess and defect are epsilon_+ = 4.51% +/- 0.03% and epsilon_- = -2.44% +/- 0.02%. Thus BF Ara is yet another in-the-gap nova with mass ratio q of around 0.21.