| 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. |
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@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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