Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VIII: The Eighth Year (2015-2016)
astro-ph.SR
/ Authors
Taichi Kato, Franz-Josef Hambsch, Berto Monard, Tonny Vanmunster, Yutaka Maeda, Ian Miller, Hiroshi Itoh, Seiichiro Kiyota, Keisuke Isogai, Mariko Kimura
and 68 more authors
Akira Imada, Tamas Tordai, Hidehiko Akazawa, Kenji Tanabe, Noritoshi Otani, Minako Ogi, Kazuko Ando, Naoki Takigawa, Pavol A. Dubovsky, Igor Kudzej, Sergey Yu. Shugarov, Natalia Katysheva, Polina Golysheva, Natalia Gladilina, Drahomir Chochol, Peter Starr, Kiyoshi Kasai, Roger D. Pickard, Enrique de Miguel, Naoto Kojiguchi, Yuki Sugiura, Daiki Fukushima, Eiji Yamada
/ Abstract
Continuing the project described by Kato et al. (2009, arXiv:0905.1757), 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, 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, 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, SDSS J074859.55+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 (~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 the future observations will be more astrophysically beneficial and rewarding to observers, we propose guidelines how to organize observations of various superoutbursts.