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Study of negative and positive superhumps in ER Ursae Majoris

机译：ER Ursae Majoris的负尖峰和正尖峰研究

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We carried out photometric observations of the SUUMa-type dwarf nova ERUMa during 2011 and 2012, which showed the existence of persistent negative superhumps even during the superoutburst. We performed a two-dimensional period analysis of its light curves by using a method called "least absolute shrinkage and selection operator" (Lasso) and the "phase dispersion minimization" (PDM) analysis, and found that the period of negative superhumps systematically changed between a superoutburst and the next superoutburst. The trend of the period change can be interpreted as a reflection of the change of the disk radius. This change is in agreement with the one predicted by the thermal tidal instability model. The normal outburst during a supercycle showed a general trend that the rising rate to its maximum becomes slower as the next superoutburst is approaching. The change can be interpreted as the consequence of the increased gas-stream flow into the inner region of the disk as a result of the tilted disk. Some of superoutbursts were found to be triggered by a precursor normal outburst when the positive superhump appeared to develop. The positive and negative superhumps coexisted during the superoutburst. Positive superhumps were prominent only for four or five days after the supermaximum, while the signal of negative superhumps became stronger after the middle phase of the superoutburst plateau. A simple combination of the positive and negative superhumps was found to be insufficient for reproduction of the complex profile variation. We were able to detect the developing phase of positive superhumps (stage A superhumps) for the first time in ER UMa-type dwarf novae. Using the period of stage A superhumps, we obtained a mass ratio of 0.100(15), which indicates that ERUMa is on the ordinary evolutional track of cataclysmic variable stars.
机译：我们在2011年和2012年对SUUMa型矮新星ERUMa进行了光度学观察，结果表明即使在超爆发期间也存在持续的负超隆。我们使用“最小绝对收缩和选择算子”（Lasso）和“相散最小化”（PDM）分析方法对其光曲线进行了二维周期分析，发现负超级峰的周期系统地改变了在一次超级爆发与下一次超级爆发之间。周期变化的趋势可以解释为磁盘半径变化的反映。这一变化与潮汐热不稳定模型预测的变化一致。在超级周期内的正常爆发显示出总体趋势，即随着下一次超级爆发的临近，上升至最大速率的速度变慢。该变化可以解释为由于倾斜的盘而导致流入盘的内部区域的气流增加的结果。当出现正的超级驼峰时，发现一些超级爆发是由前兆正常爆发触发的。正爆发和负爆发在超爆发期间共存。正超峰仅在超最大值出现后的四到五天内出现，而负超峰的信号在超爆发高原的中期阶段之后变得更强。发现正负超峰的简单组合不足以再现复杂的轮廓变化。我们能够在ER UMa型矮新星中首次检测到正超级驼峰的发育阶段（阶段A超级驼峰）。使用阶段A的超级驼峰，我们获得的质量比为0.100（15），这表明ERUMa处于大变变星的普通演化轨道上。

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