Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. III. The Third Year (2010–2011)

• DOI: 10.1093/pasj/64.1.21
• Publication Date: 2014-03-07T18:33:15Z
• Authors: Taichi Kato; Hiroyuki Maehara; Ian Miller; Tomohito Ohshima; Enrique de Miguel; Kenji Tanabe; Kazuyoshi Imamura; Hidehiko Akazawa; Nanae Kunitomi; Ryosuke Takagi; Mikiha Nose; Franz-Josef Hambsch; Seiichiro Kiyota; Elena P. Pavlenko; Aleksei V. Baklanov; Oksana I. Antonyuk; Denis Samsonov; Aleksei Sosnovskij; Kirill Antonyuk; Maksim V. Andreev; Etienne Morelle; Pavol A. Dubovsky; Igor Kudzej; Arto Oksanen; Gianluca Masi; Thomas Krajci; Roger D. Pickard; Richard Sabo; Hiroshi Itoh; William Stein; Shawn Dvorak; Arne Henden; Shinichi Nakagawa; Ryo Noguchi; Eriko Iino; Katsura Matsumoto; Hiroki Nishitani; Tomoya Aoki; Hiroshi Kobayashi; Chihiro Akasaka; Greg Bolt; Jeremy Shears; Javier Ruiz; Sergey Yu. Shugarov; Drahomir Chochol; Nikolai A. Parakhin; Berto Monard; Kazuhiko Shiokawa; Kiyoshi Kasai; Bart Staels; Atsushi Miyashita; Donn R. Starkey; Yenal Ögmen; Colin Littlefield; Natalia Katysheva; Ivan M. Sergey; Denis Denisenko; Tamas Tordai; Robert Fidrich; Vitaly P. Goranskij; Jani Virtanen; Tim Crawford; Jochen Pietz; Robert A. Koff; David Boyd; Steve Brady; Nick James; William N. Goff; Koh-ichi Itagaki; Hideo Nishimura; Youichirou Nakashima; Seiichi Yoshida; Rod Stubbings; Gary Poyner; Yutaka Maeda; Stanislav A. Koro...; Kirill V. Sokolovsky; Seiji Ueda
• Keywords: Accretion disc; Dwarf nova; Orbital period

Abstract Continuing the project described by Kato et al. (2009, PASJ, 61, S395), we collected times of superhump maxima for 51 SU UMa-type dwarf novae, mainly observed during 2010–2011 season. Although most new data systems with short periods basically confirmed findings (ibid.) and (2010, 62, 1525), long-period system GX Cas showed an exceptionally large positive-period derivative. An analysis public Kepler V344 Lyr V1504 Cyg yielded less-striking stage transitions. In Lyr, there was a prominent secondary component growing late superoutbursts, this persisted at least two more cycles successive normal outbursts. We also investigated superoutburst conspicuous eclipsing objects: HT WZ Sge-type object SDSS J080434.20$+$510349.2. Strong beat phenomena were detected in both objects, late-stage superhumps latter had almost constant luminosity repeated rebrightenings. The J133941.11$+$484727.5 phase reversal around rapid fading from superoutburst. phenomenon, even after end A pilot study amplitudes indicated that amplitude is strongly correlated orbital period, dependence on inclination weak inclinations smaller than 80$^{\circ}$.