Please use this identifier to cite or link to this item: https://www.um.edu.mt/library/oar/handle/123456789/111256
Title: 2021 superoutburst of the WZ Sge-type dwarf nova V627 Pegasi lacks an early superhump phase
Authors: Tampo, Yusuke
Kato, Taichi
Kojiguchi, Naoto
Shugarov, Sergey Yu
Itoh, Hiroshi
Matsumoto, Katsura
Nakagawa, Momoka
Nishida, Yukitaka
Richmond, Michael
Shibata, Masaaki
Ito, Junpei
Kokhirova, Gulchehra
Rakhmatullaeva, Firuza
Tordai, Tamas
Kiyota, Seiichiro
Ruiz, Javier
Dubovsky, Pavol A
Medulka, Tomas
Pavlenko, Elena P
Antonyuk, Oksana I
Sosnovskij, Aleksei A
Baklanov, Aleksei V
Krushevska, Viktoriia
Vanmunster, Tonny
Brincat, Stephen
Petrik, Karol
Galdies, Charles
Hambsch, Franz-Josef
Maeda, Yutaka
Nogami, Daisaku
Keywords: Dwarf novae
Cataclysmic variable stars
Variable stars
Dwarf stars
Issue Date: 2023
Publisher: Oxford University Press
Citation: Tampo, Y., Kato, T., Kojiguchi, N., Shugarov, S. Y., Itoh, H., Matsumoto, K.,...Nogami, D. (2023). 2021 superoutburst of the WZ Sge-type dwarf nova V627 Pegasi lacks an early superhump phase. Publications of the Astronomical Society of Japan, 75(3), 619-633.
Abstract: Superoutbursts in WZ Sge-type dwarf novae (DNe) are characterized by both early superhumps and ordinary superhumps originating from the 2 : 1 and 3 : 1 resonances, respectively. However, some WZ Sge-type DNe show a superoutburst lacking early superhumps; it is not well established how these differ from superoutbursts with an early superhump phase. We report time-resolved photometric observations of the WZ Sge-type DN V627 Peg during its 2021 superoutburst. The detection of ordinary superhumps before the superoutburst peak highlights that this 2021 superoutburst of V627 Peg, like that in 2014, did not feature an early superhump phase. The duration of stage B superhumps was slightly longer in the 2010 superoutburst accompanied by early superhumps than that in the 2014 and 2021 superoutbursts, which lacked early superhumps. This result suggests that an accretion disk experiencing the 2 : 1 resonance may have a larger mass at the inner part of the disk and hence needs more time for the inner disk to become eccentric. The presence of a precursor outburst in the 2021 superoutburst suggests that the maximum disk radius should be smaller than that of the 2014 superoutburst, even though the duration of quiescence was longer than that before the 2021 superoutburst. This could be accomplished if the 2021 superoutburst was triggered as an inside-out outburst or if the mass transfer rate in quiescence changes by a factor of two, suggesting that the outburst mechanism and quiescence state of WZ Sge-type DNe may have more variety than ever thought.
URI: https://www.um.edu.mt/library/oar/handle/123456789/111256
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