Superoutburst of CR Bootis: Estimation of mass ratio of a
typical AM CVn star by stage A superhumps

J 2016

Superoutburst of CR Bootis: Estimation of mass ratio of a typical AM CVn star by stage A superhumps

ISOGAI, Keisuke; Taichi KATO; Tomohito OHSHIMA; Kiyoshi KASAI; Arto OKSANEN et al.

Základní údaje

Originální název

Superoutburst of CR Bootis: Estimation of mass ratio of a typical AM CVn star by stage A superhumps

Autoři

Vydání

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, OXFORD, OXFORD UNIV PRESS, 2016, 0004-6264

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Velká Británie a Severní Irsko

Utajení

není předmětem státního či obchodního tajemství

Odkazy

URL

Impakt faktor

Impact factor: 1.972

Označené pro přenos do RIV

Ano

Kód RIV

RIV/00216224:14310/16:00093558

Organizační jednotka

Přírodovědecká fakulta

Klíčová slova anglicky

accretion; accretion disks; novae; cataclysmic variables; stars; dwarf novae; stars; individual (CR Bootis)

Štítky

AKR, rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 14. 4. 2017 11:24, Ing. Andrea Mikešková

Anotace

V originále

We report on two superoutbursts of the AM CVn-type object CR Boo in 2014 April-March and 2015 May-June. A precursor outburst accompanied both of these superoutbursts. During the rising branch of the main superoutburst in 2014, we detected growing super-humps (stage A superhumps) whose period was 0.017669(24) d. Assuming that this period reflects the dynamical precession rate at the radius of the 3: 1 resonance, we could estimate the mass ratio (q = M-2/M-1) of 0.101(4) by using the stage A superhump period and the orbital period of 0.0170290(6) d. This mass ratio is consistent with that expected from the theoretical evolutionary model of AM CVn-type objects. The detection of precursor outbursts and stage A superhumps is the second case in AM CVn-type objects. There are two interpretations of the outbursts of AM CVn-type objects. One is a dwarf nova (DN) outbursts analogy, which suggets that the outbursts are caused by thermal and tidal instabilities. Another is the VY Scl-type variation, which suggests that the outbursts are caused by the variation of the mass-transfer rate of the secondary. This detection of the superhump variations strongly supports the former interpretation.

Citovat

ISOGAI, Keisuke; Taichi KATO; Tomohito OHSHIMA; Kiyoshi KASAI; Arto OKSANEN; Kazunari MASUMOTO; Daiki FUKUSHIMA; Kazuki MAEDA; Miho KAWABATA; Risa MATSUDA; Naoto KOJIGUCHI; Yuki SUGIURA; Nao TAKEDA; Katsura MATSUMOTO; Hiroshi ITOH; Elena P. PAVLENKO; Kirill ANTONYUK; Oksana ANTONYUK; Nikolai PIT; Aleksei SOSNOVSKIJ; Alex BAKLANOV; Julia BABINA; Aleksandr SKLYANOV; Seiichiro KIYOTA; Franz-Josef HAMBSCH; Colin LITTLEFIELD; Yutaka MAEDA; Lewis M. COOK; Gianluca MASI; Pavol A. DUBOVSKY; Rudolf NOVÁK; Shawn DVORAK; Akira IMADA a Daisaku NOGAMI. Superoutburst of CR Bootis: Estimation of mass ratio of a typical AM CVn star by stage A superhumps. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN. OXFORD: OXFORD UNIV PRESS, 2016, roč. 68, č. 4, s. "nestrankovano", 9 s. ISSN 0004-6264. Dostupné z: https://doi.org/10.1093/pasj/psw063.

@article{1372593,
   author = {Isogai, Keisuke and Kato, Taichi and Ohshima, Tomohito and Kasai, Kiyoshi and Oksanen, Arto and Masumoto, Kazunari and Fukushima, Daiki and Maeda, Kazuki and Kawabata, Miho and Matsuda, Risa and Kojiguchi, Naoto and Sugiura, Yuki and Takeda, Nao and Matsumoto, Katsura and Itoh, Hiroshi and Pavlenko, Elena P. and Antonyuk, Kirill and Antonyuk, Oksana and Pit, Nikolai and Sosnovskij, Aleksei and Baklanov, Alex and Babina, Julia and Sklyanov, Aleksandr and Kiyota, Seiichiro and Hambsch, FranzandJosef and Littlefield, Colin and Maeda, Yutaka and Cook, Lewis M. and Masi, Gianluca and Dubovsky, Pavol A. and Novák, Rudolf and Dvorak, Shawn and Imada, Akira and Nogami, Daisaku},
   article_location = {OXFORD},
   article_number = {4},
   doi = {https://doi.org/10.1093/pasj/psw063},
   keywords = {accretion; accretion disks; novae; cataclysmic variables; stars; dwarf novae; stars; individual (CR Bootis)},
   language = {eng},
   issn = {0004-6264},
   journal = {PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN},
   title = {Superoutburst of CR Bootis: Estimation of mass ratio of a typical AM CVn star by stage A superhumps},
   url = {https://academic.oup.com/pasj/article-abstract/68/4/64/2223334/Superoutburst-of-CR-Bootis-Estimation-of-mass?redirectedFrom=fulltext},
   volume = {68},
   year = {2016}
}

TY  - JOUR
ID  - 1372593
AU  - Isogai, Keisuke - Kato, Taichi - Ohshima, Tomohito - Kasai, Kiyoshi - Oksanen, Arto - Masumoto, Kazunari - Fukushima, Daiki - Maeda, Kazuki - Kawabata, Miho - Matsuda, Risa - Kojiguchi, Naoto - Sugiura, Yuki - Takeda, Nao - Matsumoto, Katsura - Itoh, Hiroshi - Pavlenko, Elena P. - Antonyuk, Kirill - Antonyuk, Oksana - Pit, Nikolai - Sosnovskij, Aleksei - Baklanov, Alex - Babina, Julia - Sklyanov, Aleksandr - Kiyota, Seiichiro - Hambsch, Franz-Josef - Littlefield, Colin - Maeda, Yutaka - Cook, Lewis M. - Masi, Gianluca - Dubovsky, Pavol A. - Novák, Rudolf - Dvorak, Shawn - Imada, Akira - Nogami, Daisaku
PY  - 2016
TI  - Superoutburst of CR Bootis: Estimation of mass ratio of a typical AM CVn star by stage A superhumps
JF  - PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
VL  - 68
IS  - 4
SP  - "nestrankovano"
EP  - "nestrankovano"
PB  - OXFORD UNIV PRESS
SN  - 00046264
KW  - accretion
KW  - accretion disks
KW  - novae
KW  - cataclysmic variables
KW  - stars
KW  - dwarf novae
KW  - stars
KW  - individual (CR Bootis)
UR  - https://academic.oup.com/pasj/article-abstract/68/4/64/2223334/Superoutburst-of-CR-Bootis-Estimation-of-mass?redirectedFrom=fulltext
L2  - https://academic.oup.com/pasj/article-abstract/68/4/64/2223334/Superoutburst-of-CR-Bootis-Estimation-of-mass?redirectedFrom=fulltext
N2  - We report on two superoutbursts of the AM CVn-type object CR Boo in 2014 April-March and 2015 May-June. A precursor outburst accompanied both of these superoutbursts. During the rising branch of the main superoutburst in 2014, we detected growing super-humps (stage A superhumps) whose period was 0.017669(24) d. Assuming that this period reflects the dynamical precession rate at the radius of the 3: 1 resonance, we could estimate the mass ratio (q = M-2/M-1) of 0.101(4) by using the stage A superhump period and the orbital period of 0.0170290(6) d. This mass ratio is consistent with that expected from the theoretical evolutionary model of AM CVn-type objects. The detection of precursor outbursts and stage A superhumps is the second case in AM CVn-type objects. There are two interpretations of the outbursts of AM CVn-type objects. One is a dwarf nova (DN) outbursts analogy, which suggets that the outbursts are caused by thermal and tidal instabilities. Another is the VY Scl-type variation, which suggests that the outbursts are caused by the variation of the mass-transfer rate of the secondary. This detection of the superhump variations strongly supports the former interpretation.
ER  -

ISOGAI, Keisuke; Taichi KATO; Tomohito OHSHIMA; Kiyoshi KASAI; Arto OKSANEN; Kazunari MASUMOTO; Daiki FUKUSHIMA; Kazuki MAEDA; Miho KAWABATA; Risa MATSUDA; Naoto KOJIGUCHI; Yuki SUGIURA; Nao TAKEDA; Katsura MATSUMOTO; Hiroshi ITOH; Elena P. PAVLENKO; Kirill ANTONYUK; Oksana ANTONYUK; Nikolai PIT; Aleksei SOSNOVSKIJ; Alex BAKLANOV; Julia BABINA; Aleksandr SKLYANOV; Seiichiro KIYOTA; Franz-Josef HAMBSCH; Colin LITTLEFIELD; Yutaka MAEDA; Lewis M. COOK; Gianluca MASI; Pavol A. DUBOVSKY; Rudolf NOVÁK; Shawn DVORAK; Akira IMADA a Daisaku NOGAMI. Superoutburst of CR Bootis: Estimation of mass ratio of a typical AM CVn star by stage A superhumps. \textit{PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN}. OXFORD: OXFORD UNIV PRESS, 2016, roč.~68, č.~4, s.~''nestrankovano'', 9 s. ISSN~0004-6264. Dostupné z: https://doi.org/10.1093/pasj/psw063.

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