MASTER OT J030227.28+191754.5: an unprecedentedly energetic dwarf nova outburst
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2024
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| author | 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 Jr, 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 |
| author_facet | 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 Jr, 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 |
| contents | 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) the double-peaked optical emission lines, and (2) the early and ordinary superhumps, established that 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 as 0.05986(1) d and 0.063(1), respectively. These are within a typical range of low-mass-ratio DNe. 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 $\simeq$ 10$^{20}$ g s$^{-1}$ to explain its peak optical luminosity and (2) large mass was stored in the disk at the outburst onset. These cannot be explained solely by the impact of its massive ($\gtrsim$ 1.15 M$_\odot$) primary white dwarf implied by Kimura et al. (2023). Instead, we propose that the probable origin of this enormously energetic DN outburst is the even lower quiescence viscosity than other WZ Sge-type DNe. This discussion is qualitatively valid for most possible binary parameter spaces unless the inclination is low ($\lesssim 40^\circ$) 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 maximum showed the strong emission lines of Balmer, He I, and He II series whose core is narrower than $\sim 800$ km s$^{-1}$. Considering its binary parameters, a Keplerian disk cannot explain this narrow component, but the presumable origin is disk winds. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_13783 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | MASTER OT J030227.28+191754.5: an unprecedentedly energetic dwarf nova outburst 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 Jr, 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 Solar and Stellar Astrophysics High Energy Astrophysical Phenomena 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) the double-peaked optical emission lines, and (2) the early and ordinary superhumps, established that 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 as 0.05986(1) d and 0.063(1), respectively. These are within a typical range of low-mass-ratio DNe. 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 $\simeq$ 10$^{20}$ g s$^{-1}$ to explain its peak optical luminosity and (2) large mass was stored in the disk at the outburst onset. These cannot be explained solely by the impact of its massive ($\gtrsim$ 1.15 M$_\odot$) primary white dwarf implied by Kimura et al. (2023). Instead, we propose that the probable origin of this enormously energetic DN outburst is the even lower quiescence viscosity than other WZ Sge-type DNe. This discussion is qualitatively valid for most possible binary parameter spaces unless the inclination is low ($\lesssim 40^\circ$) 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 maximum showed the strong emission lines of Balmer, He I, and He II series whose core is narrower than $\sim 800$ km s$^{-1}$. Considering its binary parameters, a Keplerian disk cannot explain this narrow component, but the presumable origin is disk winds. |
| title | MASTER OT J030227.28+191754.5: an unprecedentedly energetic dwarf nova outburst |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2408.13783 |