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arXiv:2104.04948v1, et al., We present spectroscopic and photometric observations of 17 dwarf-nova superoutbursts obtained by KOOLS-IFU mounted on the 3.8 m telescope Seimei at the Okayama Observatory of Kyoto University and through the Variable Star Network collaboration (VSNET). Our spectroscopic observations for six outbursts were performed within 1 d of their optical peak. 11 objects (TCP J00590972+3438357, ASASSN-19ado, TCP J06073081−0101501, ZTF20aavnpug, ASASSN-19ady, MASTER OT J061642.05+435617.9, TCP J20034647+1335125, ASASSN-20kv, ASASSN-20kw, MASTER OT J213908.79+161240.2, and ASASSN-20mf) were previously unknown systems, and our observations enabled quick classification of their transient type. These results illustrate that the Seimei telescope has the capability to conduct quick follow-up observations of unknown transients. Our photometric observations yielded that 11 of the objects are WZ Sge-type dwarf novae and their candidates, and the other six are SU UMa-type dwarf novae and their candidates. The He ii 4686 Å emission line was clearly detected among ASASSN-19ado, TCP J06073081−0101501 and MASTER OT J213908.79+161240.2, the association of which with a spiral arm structure in an accretion disk has been suggested in previous studies. Our result suggests that a higher-inclination system shows a stronger emission line of He ii 4686 Å, as well as larger-amplitude early superhumps., Maeda acknowledges support from the Japan Society for the Promotion of Science (JSPS) KAKENHI grant JP18H05223, JP20H00174, and JP20H04737. U. Burgaz acknowledges the support provided by the Turkish Scientific and Technical Research Council (TÜBITAK2211C and 2214A). This work was supported by the project APVV-15-0458 “Interacting binaries - Key for the Understanding of the Universe”. This work was supported by the Slovak Research and Development Agency under the contract No. APVV15-0458 and by the Slovak Academy of Sciences grant VEGA No. 2/0030/21. The authors from Sternberg institute thank the Program of Development of Lomonosov MSU ‘Leading Scientific Schools’. A.A.B, N.P.I. and M.A.B. (SAI MSU) are supported by the Interdisciplinary Scientific and Educational School of Moscow University ’Fundamental and Applied Space Research’. This research was partly supported by the Slovak Academy of Sciences grant VEGA No. 2/0030/21.

Bu tezde, kataklismik değişen yıldızların WZ Sge türü cüce novaların genel özellikleri incelenmiştir. WZ Sge sisteminin uzun dönemli ve kısa dönemli ışık değişimlerini çalışmak amacıyla TÜBİTAK Ulusal Gözlemevi (TUG) T60 ve T100 teleskopları kullanılarak WZ Sge sistemi gözlenmiştir. Bu tür sistemlerde gözlenen ışık değişimlerinin ardındaki olası mekanizmalar literatürden derlenerek özet halinde sunulmuştur. Ayrıca TUG teleskopları kullanılarak PX And nova benzeri değişen de gözlenmiş elde edilen ışık değişimleri sunulmuştur., In this thesis, general behaviors of WZ Sge type cataclysmic variables are investigated. To study long-term and short-term light variations of WZ Sge, it was observed with TÜBİTAK National Observatory (TUG) T60 and T100 telescopes. The possible mechanisms that causes these variations are summarized from the literature. In addition, a nova like variable PX And was observed with TUG telescopes and its light variations are also presented.

The WZ Sge type stars is a rare subclass of the cataclysmic variables (CVs). It possesses the properties of both dwarf novae and recurrent novae. The WZ Sge stars have the shortest orbital periods (typically 80 - 90 minutes) known among the dwarf novae, and the long (decades) recurrent time of outbursts never displayed by the dwarf novae but that is typical for the recurrent novae. At the same time the WZ Sge stars show their own unique peculiarities and are the promising objects for search for the brown dwarfs in close binaries. The brief review of the main characters of the known WZ Sge stars is given including the last results of the newly discovered and investigated binaries of this type.