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Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae

机译：SU UMa型矮新星超级驼峰的周期变化研究

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We systematically surveyed period variations of superhumps in SU UMa-type dwarf novae based on newly obtained data and past publications. In many systems, the evolution of the superhump period is found to be composed of three distinct stages: an early evolutionary stage with a longer superhump period, a middle stage with systematically varying periods, and a final stage with a shorter, stable superhump period. During the middle stage, many systems with superhump periods of less than 0.08 d show positive period derivatives. We present observational characteristics of these stages and give greatly improved statistics. Contrary to an earlier claim, we found no clear evidence for a variation of period derivatives among different superoutbursts of the same object. We present an interpretation that the lengthening of the superhump period is a result of the outward propagation of an eccentricity wave, which is limited by the radius near the tidal truncation. We interpret that late-stage superhumps are rejuvenated excitation of a 3:1 resonance when superhumps in the outer disk are effectively quenched. The general behavior of the period variation, particularly in systems with short orbital periods, appears to follow a scenario proposed in Kato, Maehara, and Monard (2008, PASJ, 60, L23). We also present an observational summary of WZ Sge-type dwarf novae. Many of them have shown long-enduring superhumps during a post-superoutburst stage having longer periods than those during the main superoutburst. The period derivatives in WZ Sge-type dwarf novae are found to be strongly correlated with the fractional superhump excess, or consequently with the mass ratio. WZ Sge-type dwarf novae with a long-lasting rebrightening or with multiple rebrightenings tend to have smaller period derivatives, and are excellent candidates for those systems around or after the period minimum of evolution of cataclysmic variables
机译：我们根据最新获得的数据和以往的出版物，系统地调查了SU UMa型矮新星中超级驼峰的周期变化。在许多系统中，发现超级驼峰期的演变由三个不同的阶段组成：超级驼峰期较长的早期进化阶段，周期性变化的中间阶段以及超级驼峰期较短，稳定的最终阶段。在中间阶段，许多超级驼峰周期小于0.08 d的系统显示正周期导数。我们介绍了这些阶段的观测特征，并给出了大大改善的统计数据。与先前的说法相反，我们没有找到明确的证据来证明同一对象的不同超爆发之间的周期导数有差异。我们提出一种解释，即超级驼峰周期的延长是偏心波向外传播的结果，该偏心波受到潮汐截断附近半径的限制。我们解释说，当外部磁盘中的超级驼峰被有效淬灭时，后期的超级驼峰会激发3：1的共振。周期变化的一般行为，尤其是在具有短轨道周期的系统中，似乎遵循加藤，前原和蒙纳德提出的设想（2008，PASJ，60，L23）。我们还介绍了WZ Sge型矮新星的观测摘要。他们中的许多人在爆发后阶段都表现出长期持久的超级隆起，其周期要长于主要爆发期间。发现WZ Sge型矮新星的周期导数与分数超驼峰过量或质量比密切相关。 WZ Sge型矮化新星具有持久的增亮作用或具有多次增亮作用，往往具有较小的周期导数，并且对于那些在催化变化最小的周期左右或之后最小的周期的系统来说，是极好的候选者

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