Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VII: The Seventh Year (2014-2015)
Taichi Kato, Franz-Josef Hambsch, Pavol A. Dubovsky, Igor Kudzej,, Berto Monard, Ian Miller, Hiroshi Itoh, Seiichiro Kiyota, Kazunari Masumoto,, Daiki Fukushima, Hiroki Kinoshita, Kazuki Maeda, Jyunya Mikami, Risa Matsuda,, Naoto Kojiguchi, Miho Kawabata, Megumi Takenaka

TL;DR
This survey compiles and analyzes superhump data from 102 SU UMa-type dwarf novae during 2014-2015, revealing statistical distributions, period features, and new insights into dwarf nova subtypes and superoutburst behaviors.
Contribution
It provides an extensive, updated statistical analysis of superhump periods, confirms the period minimum, and identifies new features in dwarf novae, including AM CVn-type objects and superoutburst variations.
Findings
Confirmed period minimum at 0.053 days.
Detected superhumps in three AM CVn-type dwarf novae.
Identified systematic supercycle variations of ~20% in some systems.
Abstract
Continuing the project described by Kato et al. (2009, arXiv:0905.1757), we collected times of superhump maxima for 102 SU UMa-type dwarf novae observed mainly during the 2014-2015 season and characterized these objects. Our project has greatly improved the statistics of the distribution of orbital periods, which is a good approximation of the distribution of cataclysmic variables at the terminal evolutionary stage, and confirmed the presence of a period minimum at a period of 0.053 d and a period spike just above this period. The number density monotonically decreased toward the longer period and there was no strong indication of a period gap. We detected possible negative superhumps in Z Cha. It is possible that normal outbursts are also suppressed by the presence of a disk tilt in this system. There was no indication of enhanced orbital humps just preceding the superoutburst, and…
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