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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Analysis of a kepler light curve of the novalike cataclysmic variable KIC 8751494
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Analysis of a kepler light curve of the novalike cataclysmic variable KIC 8751494

机译：新星型催化变量KIC 8751494的开普勒光曲线分析

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摘要

We analyzed a Kepler light curve of KIC 8751494, a recently recognized novalike cataclysmic variable in the Kepler field. We detected a stable periodicity of 0.114379(1) d, which we identified as being the binary's orbital period. The stronger photometric period at around 0.12245 d, which had been detected from a ground-based observation, was found to be variable, and we identified this period as the positive-superhump period. This superhump period showed short-term (10-20 d) strong variations in period most unexpectedly when the object entered a slightly faint state. The fractional superhump excess varied by as much large as ?30%. The variation of the period very well traced the variation of the brightness of the system. The time-scale of this variation of superhump periods was too slow to be interpreted as a variation caused by a change of the disk radius due to thermal disk instability. We interpreted the cause of the period variation as a varying pressure effect on the period of positive superhumps. This finding suggests that the pressure effect, in at least novalike systems, plays a very important (up to ?30% in the precession rate) role in producing the period of positive superhumps. We also described a possible detection of negative superhumps with a varying period of 0.1071-0.1081 d in the Q14 run of the Kepler data, and found that the variation of frequency of negative superhumps followed that of positive superhumps. The relation between the fractional superhump excesses of negative and positive superhumps can be understood if the angular frequency of positive superhumps is decreased by a pressure effect. We also found that the phase of the variation in the velocity of the emission lines reported in the earlier study is compatible with the SWSex-type classification. Further, we introduced a new two-dimentional period analysis using least absolute shrinkage and selection operator (Lasso), and showed superior advantages of this method.
机译：我们分析了KIC 8751494的开普勒光曲线，KIC 8751494是开普勒场中最近被认可的新星状催化变量。我们检测到一个稳定的周期0.114379（1）d，我们将其确定为二进制的轨道周期。通过地面观测发现，在约0.12245 d处较强的光度周期是可变的，因此我们将该时间段确定为正超驼峰期。当物体进入微弱的状态时，这个超驼峰期表现出短期（10-20 d）的强烈变化。超级驼峰的分数过量变化高达30％。周期的变化很好地追踪了系统亮度的变化。超级驼峰周期的这种变化的时间尺度太慢，以至于不能解释为由于热磁盘不稳定而引起的磁盘半径变化所引起的变化。我们将周期变化的原因解释为正超驼峰周期的压力变化。这一发现表明，至少在新星系统中，压力效应在产生正超级驼峰期间起着非常重要的作用（进动率高达30％）。我们还描述了在开普勒数据的Q14运行中以0.1071-0.1081 d的变化周期检测负超峰的可能性，并发现负超峰的频率变化跟随正超峰的变化。如果正超级峰的角频率通过压力效应而减小，则可以理解负超级峰与正超级峰的分数超级峰之间的关系。我们还发现，在较早的研究中报告的发射线速度变化的相位与SWSex类型分类兼容。此外，我们介绍了一种使用最小绝对收缩和选择算子（Lasso）的新的二维周期分析，并显示了该方法的优越性。

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