RZ Leonis Minoris bridging between ER Ursae Majoris-Type dwarf nova & nova-like system

Taichi Kato; Ryoko Ishioka; Keisuke Isogai; Mariko Kimura; Akira Imada; Ian Miller; Kazunari Masumoto; Hirochika Nishino; Naoto Kojiguchi; Miho Kawabata; Daisuke Sakai; Yuki Sugiura; Hisami Furukawa; Kenta Yamamura; Hiroshi Kobayashi; Katsura Matsumoto; Shiang Yu Wang; Yi Chou; Chow Choong Ngeow; Wen Ping Chen; Neelam Panwar; Chi Sheng Lin; Hsiang Yao Hsiao; Jhen Kuei Guo; Chien Cheng Lin; Chingis Omarov; Anatoly Kusakin; Maxim Krugov; Donn R. Starkey; Elena P. Pavlenko; Kirill A. Antonyuk; Aleksei A. Sosnjvskij; Oksana I. Antonyuk; Nikolai V. Pit; Alex V. Baklanov; Julia V. Babina; Hiroshi Itoh; Stefano Padovan; Hidehiko Akazawa; Stella Kafka; Enrique De Miguel; Roger D. Pickard; Seiichiro Kiyota; Sergey Yu Shugarov; Drahomir Chochol; Viktoriia Krushevska; Matej Seker ǎs; Olga Pikalova; Richard Sabo; Pavol A. Dubovsky; Igor Kudzej; Joseph Ulowetz; Shawn Dvorak; Geoff Stone; Tamás Tordai; Franky Dubois; Ludwig Logie; Steve Rau; Siegfried Vanaverbeke; Tonny Vanmunster; Arto Oksanen; Yutaka Maeda; Kiyoshi Kasai; Natalia Katysheva; Etienne Morelle; Vitaly V. Neustroev; George Sjoberg

doi:10.1093/pasj/psw101

RZ Leonis Minoris bridging between ER Ursae Majoris-Type dwarf nova & nova-like system

Taichi Kato, Ryoko Ishioka, Keisuke Isogai, Mariko Kimura, Akira Imada, Ian Miller, Kazunari Masumoto, Hirochika Nishino, Naoto Kojiguchi, Miho Kawabata, Daisuke Sakai, Yuki Sugiura, Hisami Furukawa, Kenta Yamamura, Hiroshi Kobayashi, Katsura Matsumoto, Shiang Yu Wang, Yi Chou, Chow Choong Ngeow, Wen Ping ChenNeelam Panwar, Chi Sheng Lin, Hsiang Yao Hsiao, Jhen Kuei Guo, Chien Cheng Lin, Chingis Omarov, Anatoly Kusakin, Maxim Krugov, Donn R. Starkey, Elena P. Pavlenko, Kirill A. Antonyuk, Aleksei A. Sosnjvskij, Oksana I. Antonyuk, Nikolai V. Pit, Alex V. Baklanov, Julia V. Babina, Hiroshi Itoh, Stefano Padovan, Hidehiko Akazawa, Stella Kafka, Enrique De Miguel, Roger D. Pickard, Seiichiro Kiyota, Sergey Yu Shugarov, Drahomir Chochol, Viktoriia Krushevska, Matej Seker ǎs, Olga Pikalova, Richard Sabo, Pavol A. Dubovsky, Igor Kudzej, Joseph Ulowetz, Shawn Dvorak, Geoff Stone, Tamás Tordai, Franky Dubois, Ludwig Logie, Steve Rau, Siegfried Vanaverbeke, Tonny Vanmunster, Arto Oksanen, Yutaka Maeda, Kiyoshi Kasai, Natalia Katysheva, Etienne Morelle, Vitaly V. Neustroev, George Sjoberg

天文研究所

研究成果: 雜誌貢獻 › 期刊論文 › 同行評審

15 引文斯高帕斯（Scopus）

摘要

We observed RZ LMI, which is renowned for its extremely short (∼19 d) supercycle and is a member of a small, unusual class of cataclysmic variables called ERUMa-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, and 60 d for three consecutive superoutbursts.We consider that the object virtually experienced a transition to the novalike state (permanent superhumper). This observed behavior reproduced the prediction of the thermal-Tidal instability model extremely well. 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 an orbital period of 0.05792 d, which suggests a mass ratio of 0.105(5). This relatively large mass ratio is even above that of ordinary SUUMa-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 secondary with an evolved core in a system evolving toward an AM CVn-Type object.

原文	???core.languages.en_GB???
文章編號	107
期刊	Publications of the Astronomical Society of Japan
卷	68
發行號	6
DOIs	https://doi.org/10.1093/pasj/psw101
出版狀態	已出版 - 10月 2016

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10.1093/pasj/psw101

引用此

Kato, T., Ishioka, R., Isogai, K., Kimura, M., Imada, A., Miller, I., Masumoto, K., Nishino, H., Kojiguchi, N., Kawabata, M., Sakai, D., Sugiura, Y., Furukawa, H., Yamamura, K., Kobayashi, H., Matsumoto, K., Wang, S. Y., Chou, Y., Ngeow, C. C., ... Sjoberg, G. (2016). RZ Leonis Minoris bridging between ER Ursae Majoris-Type dwarf nova & nova-like system. Publications of the Astronomical Society of Japan, 68(6), 文章 107. https://doi.org/10.1093/pasj/psw101

@article{4b5da92684a14ff5b57028ec54acace3,

title = "RZ Leonis Minoris bridging between ER Ursae Majoris-Type dwarf nova & nova-like system",

abstract = "We observed RZ LMI, which is renowned for its extremely short (∼19 d) supercycle and is a member of a small, unusual class of cataclysmic variables called ERUMa-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, and 60 d for three consecutive superoutbursts.We consider that the object virtually experienced a transition to the novalike state (permanent superhumper). This observed behavior reproduced the prediction of the thermal-Tidal instability model extremely well. 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 an orbital period of 0.05792 d, which suggests a mass ratio of 0.105(5). This relatively large mass ratio is even above that of ordinary SUUMa-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 secondary with an evolved core in a system evolving toward an AM CVn-Type object.",

keywords = "Accretion, Accretion disks-novae, Cataclysmic variables-stars: dwarf novae-stars: individual (rz leonis minoris)",

author = "Taichi Kato and Ryoko Ishioka and Keisuke Isogai and Mariko Kimura and Akira Imada and Ian Miller and Kazunari Masumoto and Hirochika Nishino and Naoto Kojiguchi and Miho Kawabata and Daisuke Sakai and Yuki Sugiura and Hisami Furukawa and Kenta Yamamura and Hiroshi Kobayashi and Katsura Matsumoto and Wang, {Shiang Yu} and Yi Chou and Ngeow, {Chow Choong} and Chen, {Wen Ping} and Neelam Panwar and Lin, {Chi Sheng} and Hsiao, {Hsiang Yao} and Guo, {Jhen Kuei} and Lin, {Chien Cheng} and Chingis Omarov and Anatoly Kusakin and Maxim Krugov and Starkey, {Donn R.} and Pavlenko, {Elena P.} and Antonyuk, {Kirill A.} and Sosnjvskij, {Aleksei A.} and Antonyuk, {Oksana I.} and Pit, {Nikolai V.} and Baklanov, {Alex V.} and Babina, {Julia V.} and Hiroshi Itoh and Stefano Padovan and Hidehiko Akazawa and Stella Kafka and {De Miguel}, Enrique and Pickard, {Roger D.} and Seiichiro Kiyota and Shugarov, {Sergey Yu} and Drahomir Chochol and Viktoriia Krushevska and ǎs, {Matej Seker} and Olga Pikalova and Richard Sabo and Dubovsky, {Pavol A.} and Igor Kudzej and Joseph Ulowetz and Shawn Dvorak and Geoff Stone and Tam{\'a}s Tordai and Franky Dubois and Ludwig Logie and Steve Rau and Siegfried Vanaverbeke and Tonny Vanmunster and Arto Oksanen and Yutaka Maeda and Kiyoshi Kasai and Natalia Katysheva and Etienne Morelle and Neustroev, {Vitaly V.} and George Sjoberg",

note = "Publisher Copyright: {\textcopyright}The Author 2016.",

year = "2016",

month = oct,

doi = "10.1093/pasj/psw101",

language = "???core.languages.en_GB???",

volume = "68",

journal = "Publications of the Astronomical Society of Japan",

issn = "0004-6264",

number = "6",

}

Kato, T, Ishioka, R, Isogai, K, Kimura, M, Imada, A, Miller, I, Masumoto, K, Nishino, H, Kojiguchi, N, Kawabata, M, Sakai, D, Sugiura, Y, Furukawa, H, Yamamura, K, Kobayashi, H, Matsumoto, K, Wang, SY, Chou, Y , Ngeow, CC , Chen, WP, Panwar, N, Lin, CS, Hsiao, HY, Guo, JK, Lin, CC, Omarov, C, Kusakin, A, Krugov, M, Starkey, DR, Pavlenko, EP, Antonyuk, KA, Sosnjvskij, AA, Antonyuk, OI, Pit, NV, Baklanov, AV, Babina, JV, Itoh, H, Padovan, S, Akazawa, H, Kafka, S, De Miguel, E, Pickard, RD, Kiyota, S, Shugarov, SY, Chochol, D, Krushevska, V, ǎs, MS, Pikalova, O, Sabo, R, Dubovsky, PA, Kudzej, I, Ulowetz, J, Dvorak, S, Stone, G, Tordai, T, Dubois, F, Logie, L, Rau, S, Vanaverbeke, S, Vanmunster, T, Oksanen, A, Maeda, Y, Kasai, K, Katysheva, N, Morelle, E, Neustroev, VV & Sjoberg, G 2016, 'RZ Leonis Minoris bridging between ER Ursae Majoris-Type dwarf nova & nova-like system', Publications of the Astronomical Society of Japan, 卷 68, 編號 6, 107. https://doi.org/10.1093/pasj/psw101

TY - JOUR

T1 - RZ Leonis Minoris bridging between ER Ursae Majoris-Type dwarf nova & nova-like system

AU - Kato, Taichi

AU - Ishioka, Ryoko

AU - Isogai, Keisuke

AU - Kimura, Mariko

AU - Imada, Akira

AU - Miller, Ian

AU - Masumoto, Kazunari

AU - Nishino, Hirochika

AU - Kojiguchi, Naoto

AU - Kawabata, Miho

AU - Sakai, Daisuke

AU - Sugiura, Yuki

AU - Furukawa, Hisami

AU - Yamamura, Kenta

AU - Kobayashi, Hiroshi

AU - Matsumoto, Katsura

AU - Wang, Shiang Yu

AU - Chou, Yi

AU - Ngeow, Chow Choong

AU - Chen, Wen Ping

AU - Panwar, Neelam

AU - Lin, Chi Sheng

AU - Hsiao, Hsiang Yao

AU - Guo, Jhen Kuei

AU - Lin, Chien Cheng

AU - Omarov, Chingis

AU - Kusakin, Anatoly

AU - Krugov, Maxim

AU - Starkey, Donn R.

AU - Pavlenko, Elena P.

AU - Antonyuk, Kirill A.

AU - Sosnjvskij, Aleksei A.

AU - Antonyuk, Oksana I.

AU - Pit, Nikolai V.

AU - Baklanov, Alex V.

AU - Babina, Julia V.

AU - Itoh, Hiroshi

AU - Padovan, Stefano

AU - Akazawa, Hidehiko

AU - Kafka, Stella

AU - De Miguel, Enrique

AU - Pickard, Roger D.

AU - Kiyota, Seiichiro

AU - Shugarov, Sergey Yu

AU - Chochol, Drahomir

AU - Krushevska, Viktoriia

AU - ǎs, Matej Seker

AU - Pikalova, Olga

AU - Sabo, Richard

AU - Dubovsky, Pavol A.

AU - Kudzej, Igor

AU - Ulowetz, Joseph

AU - Dvorak, Shawn

AU - Stone, Geoff

AU - Tordai, Tamás

AU - Dubois, Franky

AU - Logie, Ludwig

AU - Rau, Steve

AU - Vanaverbeke, Siegfried

AU - Vanmunster, Tonny

AU - Oksanen, Arto

AU - Maeda, Yutaka

AU - Kasai, Kiyoshi

AU - Katysheva, Natalia

AU - Morelle, Etienne

AU - Neustroev, Vitaly V.

AU - Sjoberg, George

PY - 2016/10

Y1 - 2016/10

N2 - We observed RZ LMI, which is renowned for its extremely short (∼19 d) supercycle and is a member of a small, unusual class of cataclysmic variables called ERUMa-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, and 60 d for three consecutive superoutbursts.We consider that the object virtually experienced a transition to the novalike state (permanent superhumper). This observed behavior reproduced the prediction of the thermal-Tidal instability model extremely well. 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 an orbital period of 0.05792 d, which suggests a mass ratio of 0.105(5). This relatively large mass ratio is even above that of ordinary SUUMa-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 secondary with an evolved core in a system evolving toward an AM CVn-Type object.

AB - We observed RZ LMI, which is renowned for its extremely short (∼19 d) supercycle and is a member of a small, unusual class of cataclysmic variables called ERUMa-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, and 60 d for three consecutive superoutbursts.We consider that the object virtually experienced a transition to the novalike state (permanent superhumper). This observed behavior reproduced the prediction of the thermal-Tidal instability model extremely well. 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 an orbital period of 0.05792 d, which suggests a mass ratio of 0.105(5). This relatively large mass ratio is even above that of ordinary SUUMa-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 secondary with an evolved core in a system evolving toward an AM CVn-Type object.

KW - Accretion

KW - Accretion disks-novae

KW - Cataclysmic variables-stars: dwarf novae-stars: individual (rz leonis minoris)

UR - http://www.scopus.com/inward/record.url?scp=85012108862&partnerID=8YFLogxK

U2 - 10.1093/pasj/psw101

DO - 10.1093/pasj/psw101

M3 - 期刊論文

AN - SCOPUS:85012108862

SN - 0004-6264

VL - 68

JO - Publications of the Astronomical Society of Japan

JF - Publications of the Astronomical Society of Japan

IS - 6

M1 - 107

ER -

RZ Leonis Minoris bridging between ER Ursae Majoris-Type dwarf nova & nova-like system

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