RZ Leonis Minoris Bridging between ER Ursae Majoris-Type Dwarf Nova and Novalike System
Creators: name: Kato, Taichi
name: Ishioka, Ryoko
name: Isogai, Keisuke
name: Kimura, Mariko
name: Imada, Akira
name: Miller, Ian
name: Masumoto, Kazunari
name: Nishino, Hirochika
name: Kojiguchi, Naoto
name: Kawabata, Miho
name: Sakai, Daisuke
name: Sugiura, Yuki
name: Furukawa, Hisami
name: Yamamura, Kenta
name: Kobayashi, Hiroshi
name: Matsumoto, Katsura
name: Wang, Shiang-Yu
name: Chou, Yi
name: Ngeow, Chow-Choong
name: Chen, Wen-Ping
name: Panwar, Neelam
name: Lin, Chi-Sheng
name: Hsiao, Hsiang-Yao
name: Guo, Jhen-Kuei
name: Lin, Chien-Cheng
name: Omarov, Chingis
name: Kusakin, Anatoly
name: Krugov, Maxim
name: Starkey, Donn R.
name: Pavlenko, Elena P.
name: Antonyuk, Kirill A.
name: Sosnjvskij, Aleksei A.
name: Antonyuk, Oksana I.
name: Pit, Nikolai V.
name: Baklanov, Alex V.
name: Babina, Julia V.
name: Itoh, Hiroshi
name: Padovan, Stefano
name: Akazawa, Hidehiko
name: Kafka, Stella
name: de Miguel, Enrique
name: Pickard, Roger D.
name: Kiyota, Seiichiro
name: Shugarov, Sergey Yu.
name: Chochol, Drahomir
name: Krushevska, Viktoriia
name: Sekeras, Matej
name: Pikalova, Olga
name: Sabo, Richard
name: Dubovsky, Pavol A.
name: Kudzej, Igor
name: Ulowetz, Joseph
name: Dvorak, Shawn
name: Stone, Geoff
name: Tordai, Tamas
name: Dubois, Franky
name: Logie, Ludwig
name: Rau, Steve
name: Vanaverbeke, Siegfried
name: Vanmunster, Tonny
name: Oksanen, Arto
name: Maeda, Yutaka
name: Kasai, Kiyoshi
name: Katysheva, Natalia
name: Morelle, Etienne
name: Neustroev, Vitaly V.
name: Sjoberg, George
Publisher: name: arXiv
Year: 2016
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We observed RZ LMi, which is renowned for the extremely (~19d) short supercycle and is a member of a small, unusual class of cataclysmic variables called ER UMa-type dwarf novae, in 2013 and 2016. In 2016, the supercycles of this object substantially lengthened in comparison to the previous measurements to 35, 32, 60d for three consecutive superoutbursts. We consider that the object virtually experienced a transition to the novalike state (permanent superhumper). This observed behavior extremely well reproduced the prediction of the thermal-tidal instability model. We detected a precursor in the 2016 superoutburst and detected growing (stage A) superhumps with a mean period of 0.0602(1)d in 2016 and in 2013. Combined with the period of superhumps immediately after the superoutburst, the mass ratio is not as small as in WZ Sge-type dwarf novae, having orbital periods similar to RZ LMi. By using least absolute shrinkage and selection operator (Lasso) two-dimensional power spectra, we detected possible negative superhumps with a period of 0.05710(1)d. We estimated the orbital period of 0.05792d, which suggests a mass ratio of 0.105(5). This relatively large mass ratio is even above ordinary SU UMa-type dwarf novae, and it is also possible that the exceptionally high mass-transfer rate in RZ LMi may be a result of a stripped core evolved secondary which are evolving toward an AM CVn-type object.
description: 14 pages, 14 figures, accepted for publication in PASJ; includes Supplementary_draft_aph.pdf with somewhat degraded figures