A high-mass-ratio red-dwarf contact binary with an extremely
cool close-in red dwarf

J 2019

A high-mass-ratio red-dwarf contact binary with an extremely cool close-in red dwarf

FANG, Xiao-Hui, Shengbang QIAN, Miloslav ZEJDA, Soonthornthum BOONRUCKSAR, Xiao ZHOU et. al.

Základní údaje

Originální název

A high-mass-ratio red-dwarf contact binary with an extremely cool close-in red dwarf

Autoři

FANG, Xiao-Hui (garant), Shengbang QIAN, Miloslav ZEJDA (203 Česká republika, domácí), Soonthornthum BOONRUCKSAR, Xiao ZHOU, Liying) ZHU a Wen Ping LIAO

Vydání

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, OXFORD, OXFORD UNIV PRESS, 2019, 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: 5.024

Kód RIV

RIV/00216224:14310/19:00113424

Organizační jednotka

Přírodovědecká fakulta

DOI

http://dx.doi.org/10.1093/pasj/psz113

UT WoS

000509666400019

Klíčová slova anglicky

binaries: close; binaries: eclipsing; stars: evolution; stars: individual (1SWASP J161335.80-284722.2)

Štítky

rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 11. 5. 2020 18:05, Mgr. Marie Šípková, DiS.

Anotace

V originále

1SWASP J161335.80-284722.2 (hereafter J161335) is an eclipsing red -dwarf binary with an orbital period of 0.229778 d, which is around the short-period limit for contact binaries. Three sets of multi -color light curves of J161335 were obtained from different telescopes in 2015 and 2016 and are analyzed using the Wilson-Devinney method. We discovered that the system is a W-type contact system with a contact degree of 19% and a high mass ratio of 0.91. By using all available eclipse times, we found that the observed - calculated (0 - C) diagram displays a cyclic oscillation with an amplitude of 0.00196(+/- 0.00006) d and a period of 4.79(+/- 0.14) yr while it undergoes a downward parabolic change. This downward variation corresponds to a continuous decrease in the orbital period at a rate of dP/dt= -4.26( 0.01) x 10(-7) d yr(-1). The small -amplitude oscillation is explained as the light travel -time effect from the gravitational influence of a third body with a lowest mass of M-3 = 0.15(+/- 0.01)M-circle dot. In solving the light curves, we found that the third light is increasing, with the wavelength suggesting that the third body may be a cool red dwarf. This is in agreement with the results obtained by analyzing the O - C diagram. The tertiary red dwarf is orbiting the central red -dwarf binary at an orbital separation of 2.8(+/- 0.2) au. These results suggest that the J161335 system may be formed through early dynamical interaction where the original low-mass component was replaced by a higher-mass third body and the lower-mass component was kicked out to a wider orbit.

Citovat

FANG, Xiao-Hui, Shengbang QIAN, Miloslav ZEJDA, Soonthornthum BOONRUCKSAR, Xiao ZHOU, Liying) ZHU a Wen Ping LIAO. A high-mass-ratio red-dwarf contact binary with an extremely cool close-in red dwarf. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN. OXFORD: OXFORD UNIV PRESS, 2019, roč. 71, č. 6, s. 1-10. ISSN 0004-6264. Dostupné z: https://dx.doi.org/10.1093/pasj/psz113.

@article{1641317,
   author = {Fang, XiaoandHui and Qian, Shengbang and Zejda, Miloslav and Boonrucksar, Soonthornthum and Zhou, Xiao and Zhu, Liying) and Liao, Wen Ping},
   article_location = {OXFORD},
   article_number = {6},
   doi = {http://dx.doi.org/10.1093/pasj/psz113},
   keywords = {binaries: close; binaries: eclipsing; stars: evolution; stars: individual (1SWASP J161335.80-284722.2)},
   language = {eng},
   issn = {0004-6264},
   journal = {PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN},
   title = {A high-mass-ratio red-dwarf contact binary with an extremely cool close-in red dwarf},
   url = {https://academic.oup.com/pasj/article-abstract/71/6/125/5587008},
   volume = {71},
   year = {2019}
}

TY  - JOUR
ID  - 1641317
AU  - Fang, Xiao-Hui - Qian, Shengbang - Zejda, Miloslav - Boonrucksar, Soonthornthum - Zhou, Xiao - Zhu, Liying) - Liao, Wen Ping
PY  - 2019
TI  - A high-mass-ratio red-dwarf contact binary with an extremely cool close-in red dwarf
JF  - PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
VL  - 71
IS  - 6
SP  - 1-10
EP  - 1-10
PB  - OXFORD UNIV PRESS
SN  - 00046264
KW  - binaries: close
KW  - binaries: eclipsing
KW  - stars: evolution
KW  - stars: individual (1SWASP J161335.80-284722.2)
UR  - https://academic.oup.com/pasj/article-abstract/71/6/125/5587008
L2  - https://academic.oup.com/pasj/article-abstract/71/6/125/5587008
N2  - 1SWASP J161335.80-284722.2 (hereafter J161335) is an eclipsing red -dwarf binary with an orbital period of 0.229778 d, which is around the short-period limit for contact binaries. Three sets of multi -color light curves of J161335 were obtained from different telescopes in 2015 and 2016 and are analyzed using the Wilson-Devinney method. We discovered that the system is a W-type contact system with a contact degree of 19% and a high mass ratio of 0.91. By using all available eclipse times, we found that the observed - calculated (0 - C) diagram displays a cyclic oscillation with an amplitude of 0.00196(+/- 0.00006) d and a period of 4.79(+/- 0.14) yr while it undergoes a downward parabolic change. This downward variation corresponds to a continuous decrease in the orbital period at a rate of dP/dt= -4.26( 0.01) x 10(-7) d yr(-1). The small -amplitude oscillation is explained as the light travel -time effect from the gravitational influence of a third body with a lowest mass of M-3 = 0.15(+/- 0.01)M-circle dot. In solving the light curves, we found that the third light is increasing, with the wavelength suggesting that the third body may be a cool red dwarf. This is in agreement with the results obtained by analyzing the O - C diagram. The tertiary red dwarf is orbiting the central red -dwarf binary at an orbital separation of 2.8(+/- 0.2) au. These results suggest that the J161335 system may be formed through early dynamical interaction where the original low-mass component was replaced by a higher-mass third body and the lower-mass component was kicked out to a wider orbit.
ER  -

FANG, Xiao-Hui, Shengbang QIAN, Miloslav ZEJDA, Soonthornthum BOONRUCKSAR, Xiao ZHOU, Liying) ZHU a Wen Ping LIAO. A high-mass-ratio red-dwarf contact binary with an extremely cool close-in red dwarf. \textit{PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN}. OXFORD: OXFORD UNIV PRESS, 2019, roč.~71, č.~6, s.~1-10. ISSN~0004-6264. Dostupné z: https://dx.doi.org/10.1093/pasj/psz113.

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