Taking advantage of the unparalleled quantity and quality of high-cadence Kepler light curves of several dwarf novae, the strength of the flickering and the high-frequency spectral index of their power spectra are investigated as a function of magnitude around the outburst cycle of these systems. Previous work suggesting that the flickering strength (on a magnitude scale) is practically constant above a given brightness threshold and only rises at fainter magnitudes is confirmed for most of the investigated systems. As a new feature, a hysteresis in the flickering strength is seen in the sense that at the same magnitude level flickering is stronger during decline from outburst than during the rise. A similar hysteresis is also seen in the spectral index. In both cases, it can qualitatively be explained under plausible assumptions within the disc instability model model for dwarf nova outbursts.

中文翻译：

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在开普勒矮新星的爆发周期中闪烁

利用几个矮新星的高频率开普勒光曲线无与伦比的数量和质量，研究了闪烁的强度和它们的功率谱的高频光谱指数，作为这些系统爆发周期周围幅度的函数. 先前的工作表明闪烁强度（在幅度上）在给定的亮度阈值之上实际上是恒定的，并且对于大多数研究的系统都证实了仅在较微弱的幅度上上升。作为一个新特征，闪烁强度的滞后被认为是在相同幅度水平下，在爆发下降期间闪烁比上升期间更强。在光谱指数中也可以看到类似的滞后现象。在这两种情况下，