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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Survey of period variations of superhumps in SU UMa-type dwarf novae. VIII. The eighth year (2015-2016)
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Survey of period variations of superhumps in SU UMa-type dwarf novae. VIII. The eighth year (2015-2016)

机译：SU UMa型矮新星超级驼峰的周期变化研究。八。第八年（2015-2016）

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摘要

Continuing the project described by Kato et al. (2009, PASJ, 61, S395), we collected times of superhump maxima for 128 SU UMa-type dwarf novae observed mainly during the 2015-2016 season and characterized these objects. The data have improved the distribution of orbital periods, the relation between the orbital period and the variation of superhumps, and the relation between period variations and the rebrightening type in WZ Sge-type objects. Coupled with new measurements of mass ratios using growing stages of superhumps, we now have a clearer and statistically greatly improved evolutionary path near the terminal stage of evolution of cataclysmic variables. Three objects (V452 Cas, KK Tel, and ASASSN-15cl) appear to have slowly growing superhumps, which is proposed to reflect the slow growth of the 3 : 1 resonance near the stability border. ASASSN-15sl, ASASSN-15ux, SDSSJ074859.55+ 312512.6, and CRTS J200331.3-284941 are newly identified eclipsing SU UMa-type (or WZ Sge-type) dwarf novae. ASASSN-15cy has a short (similar to 0.050 d) superhump period and appears to belong to EI Psc-type objects with compact secondaries having an evolved core. ASASSN-15gn, ASASSN-15hn, ASASSN-15kh, and ASASSN-16bu are candidate period bouncers with superhump periods longer than 0.06 d. We have newly obtained superhump periods for 79 objects and 13 orbital periods, including periods from early superhumps. In order that future observations will be more astrophysically beneficial and rewarding to observers, we propose guidelines on how to organize observations of various superoutbursts.
机译：继续由加藤等人描述的项目。 （2009，PASJ，61，S395），我们收集了主要在2015-2016赛季观测到的128个SU UMa型矮新星的超驼峰最大值的时间，并对这些对象进行了特征描述。这些数据改善了WZ Sge型天体的轨道周期分布，轨道周期与超驼峰变化之间的关系以及周期变化与再增亮类型之间的关系。结合使用超级驼峰生长阶段进行的质量比的新测量，我们现在在催化变量演化的最终阶段附近有了一条更清晰，统计学上显着改善的演化路径。三个对象（V452 Cas，KK Tel和ASASSN-15cl）似乎具有缓慢增长的超级峰，建议将其反映为在稳定边界附近3：1共振的缓慢增长。 ASASSN-15sl，ASASSN-15ux，SDSSJ074859.55 + 312512.6和CRTS J200331.3-284941是新发现的遮盖住SU UMa型（或WZ Sge型）的矮新星。 ASASSN-15cy具有较短的（类似于0.050 d）超跃变周期，并且似乎属于EI Psc型物体，其紧凑的次级具有演化的核。 ASASSN-15gn，ASASSN-15hn，ASASSN-15kh和ASASSN-16bu是候选周期保镖，其超驼峰周期大于0.06 d。我们新获得了79个天体和13个轨道周期的超级驼峰周期，其中包括早期超级驼峰的周期。为了使将来的观测对天文观测者更有利，并且对观测者有帮助，我们提出了有关如何组织各种超爆发观测的指南。

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