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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >The Cause of the Superoutburst in SUUMa Stars is Finally Revealed by Kepler Light Curve of V1504 Cygni
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The Cause of the Superoutburst in SUUMa Stars is Finally Revealed by Kepler Light Curve of V1504 Cygni

机译：V1504 Cygni的开普勒光曲线最终揭示了SUUMa星超爆发的原因

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We have studied the short-cadence Kepler light curve of an SUUMa star, V1504 Cyg, which covers a period of ~630 d. All superoutbursts in V1504 Cyg have turned out to be of precursor-main types, and the superhump first appears near the maximum of the precursor. The superhumps grow smoothly from the precursor to the main superoutburst, showing that the superoutburst was initiated by a tidal instability (as evidenced by the growing superhump) as envisioned in the thermal-tidal instability (TTI) model proposed by Osaki (1989, PASJ, 41, 1005). We performed a power spectral analysis of the light curve of V1504 Cyg. One of the outstanding features is the appearance of a negative superhump extending over around 300 d, well over a supercycle. We found that the appearance of the negative superhump tends to decrease the frequency of occurrence of normal outbursts. Two types of supercycles are recognized in V1504 Cyg, which are similar to those of the Type L and Type S supercycles in the light curve of VWHyi, a prototype SUUMa star, introduced by Smak (1985, Acta Astron., 35, 357). It is found that the Type L supercycle is the one accompanied by the negative superhump, and Type S is that without the negative superhump. If we adopt a tilted disk as an origin of the negative superhump, two types of the supercycles are understood to be due to a difference in the outburst interval, which is in turn caused by a difference in mass supply from the secondary to different parts of the disk. The frequency of the negative superhump varies systematically during a supercycle in V1504 Cyg. This variation can be used as an indicator of the disk-radius variation, and we have found that the observed disk-radius variation in V1504 Cyg fits very well with a prediction of the TTI model.
机译：我们研究了SUUMa恒星V1504 Cyg的短节奏开普勒光曲线，该曲线覆盖约630 d的时间。结果表明，V1504 Cyg中的所有超级爆发都是前兆为主的类型，而超级驼峰首先出现在前兆的最大值附近。超级驼峰从前兆到主要超级爆发都平稳增长，这表明超爆发是由潮汐不稳定性引发的（如不断增长的超级驼峰所证明），这是由Osaki（1989，PASJ，1991）提出的热潮汐不稳定性（TTI）模型所设想的。 41，1005）。我们对V1504 Cyg的光曲线进行了功率谱分析。杰出的特征之一是负超驼峰的出现，延伸超过300 d，超过了超轮。我们发现负超驼峰的出现倾向于降低正常爆发的发生频率。在V1504 Cyg中识别出两种类型的超级循环，这与Smak（1985，Acta Astron。，35，357）引入的SUUMa原型恒星VWHyi的光曲线中的L型和S型超级循环相似。发现L型超级循环是伴随负超级驼峰的，而S型则是没有负超级驼峰的。如果我们采用倾斜的圆盘作为负超级峰的原点，则两种超级周期被理解为是由于爆发间隔的不同而引起的，而这又是由于从次要部分到不同部分的质量供应不同而引起的。磁盘。负超级峰的频率在V1504 Cyg的超级周期中有系统地变化。该变化可以用作圆盘半径变化的指标，并且我们已经发现，在V1504 Cyg中观察到的圆盘半径变化与TTI模型的预测非常吻合。

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