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MASTER OT J030227.28+191754.5: an unprecedentedly energetic dwarf nova outburstстатья Электронная публикация
- Авторы: Tampo Yusuke, Kato Taichi, Isogai Keisuke, Kimura Mariko, Kojiguchi Naoto, Nogami Daisaku, Ito Junpei, Shibata Masaaki, Yamanaka Masayuki, Taguchi Kenta, Maehara Hiroyuki, Itoh Hiroshi, Matsumoto Katsura, Nakagawa Momoka, Nishida Yukitaka, Dvorak Shawn, Murata Katsuhiro L., Hosokawa Ryohei, Imai Yuri, Ito Naohiro, Niwano Masafumi, Sato Shota, Noto Ryotaro, Yamaguchi Ryodai, Schramm Malte, Oasa Yumiko, Kanai Takahiro, Sasaki Yu, Tordai Tamás, Vanmunster Tonny, Kiyota Seiichiro, Katysheva Nataly, Shugarov Sergey Yu, Zubareva Alexandra M., Antipin Sergei, Ikonnikova Natalia, Belinski Alexandr, Dubovsky Pavol A., Medulka Tomáš, Takahashi Jun, Takayama Masaki, Ohshima Tomohito, Saito Tomoki, Tozuka Miyako, Sako Shigeyuki, Tanaka Masaomi, Tominaga Nozomu, Horiuchi Takashi, Hanayama Hidekazu, Reichart Daniel E., Kouprianov Vladimir V., Davidson James W., Caton Daniel B., Romanov Filipp D., Lane David J., Hambsch Franz-josef, Narita Norio, Fukui Akihiko, Ikoma Masahiro, Tamura Motohide, Kawabata Koji S., Nakaoka Tatsuya, Imazawa Ryo
- Журнал: ArXiv e-prints
- Номер: 2408.13783
- Год издания: 2024
- Первая страница: 1
- Последняя страница: 24
- DOI: 10.48550/arXiv.2408.13783
- Аннотация: We present a detailed study of the MASTER OT J030227.28+191754.5 outburst in 2021-2022, reaching an amplitude of 10.2 mag and a duration of 60 d. The detections of (1) thedouble-peaked optical emission lines, and (2) the early and ordinary superhumps, establishedthat MASTER OT J030227.28+191754.5 is an extremely energetic WZ Sge-type dwarf nova(DN). Based on the superhump observations, we obtained its orbital period and mass ratio as0.05986(1) d and 0.063(1), respectively. These are within a typical range of low-mass-ratioDNe. According to the binary parameters derived based on the thermal-tidal instability model,our analyses showed that (1) the standard disk model requires an accretion rate ≃ 1020 g s−1to explain its peak optical luminosity and (2) large mass was stored in the disk at the outburstonset. These cannot be explained solely by the impact of its massive (>1.15 M⊙) primarywhite dwarf implied by Kimura et al. (2023). Instead, we propose that the probable origin ofthis enormously energetic DN outburst is the even lower quiescence viscosity than other WZSge-type DNe. This discussion is qualitatively valid for most possible binary parameter spacesunless the inclination is low (< 40◦) enough for the disk to be bright explaining the outburst amplitude. Such low inclinations, however, would not allow detectable amplitude of early superhumps in the current thermal-tidal instability model. The optical spectra at outburst maximumshowed the strong emission lines of Balmer, He I, and He II series whose core is narrower than∼ 800 km s−1. Considering its binary parameters, a Keplerian disk cannot explain this narrowcomponent, but the presumable origin is disk winds.
- Добавил в систему: Шугаров Сергей Юрьевич