A Single-lined Spectroscopic Binary Companion to an Active and Deep Contact Binary in a Quintuple Stellar System

被引:8
作者
Liao, W-P [1 ,2 ,3 ,4 ]
Qian, S-B [1 ,2 ,3 ,4 ]
Shi, X-D [1 ,2 ,3 ]
Li, L-J [1 ,2 ,3 ]
Liu, N-P [1 ,2 ,3 ]
He, J-J [1 ,2 ,3 ]
Zang, L. [1 ,2 ,3 ,4 ]
Li, P. [1 ,2 ,3 ,4 ]
机构
[1] Chinese Acad Sci, Yunnan Observ, Kunming 650216, Yunnan, Peoples R China
[2] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650216, Yunnan, Peoples R China
[3] Chinese Acad Sci, Ctr Astron Megasci, 20A Datun Rd, Beijing 100012, Peoples R China
[4] Univ Chinese Acad Sci, 19 A Yuquan Rd, Beijing, Peoples R China
基金
中国国家自然科学基金;
关键词
UNSOLVED QUADRUPLE SYSTEM; RADIAL-VELOCITY; PHYSICAL PARAMETERS; ADDITIONAL COMPONENTS; LIGHT CURVES; STARS; SEARCH;
D O I
10.3847/1538-4357/ac5038
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
V410 Aur is a known deep and low-mass-ratio contact binary with a spectroscopically tertiary component and a visual companion. However, the physical and orbital properties of the tertiary are unknown. We constructed (O - C) curve with 117 new eclipse times and those collected from the literature, which shows a cyclical variation with a period of 25.44 (+/- 1.17) yr and a projected semimajor axis of 0.0348 (+/- 0.0021) days while it undergoes a long-term period decrease at a rate of dP/dt = -1.58 x 10(-7)daysyr(-1). The cyclical variation is analyzed for the light-travel time effect. The minimum mass of the third body is determined as 1.39 (+/- 0.13) M (circle dot) that is much larger than the inferred value (0.97 M (circle dot)) of spectroscopic investigation, which indicates that the spectroscopically tertiary is a single-lined spectroscopic binary with an unseen component. The maximum orbital semimajor axis 6.19 (+/- 0.67) au of the third body is determined. Gaia detected a visual companion to V410 Aur at practically the same distance from the Sun nicely confirming the physical bond. These results reveal that V410 Aur contains a single-lined spectroscopic binary with a visual companion in a quintuple stellar system. TESS photometric solutions confirmed that V410 Aur is a deep overcontact binary with a fill-out factor of 73.83(88)% where the additional light contribution is about 24.80(18)%. The continuous variations of light curves are explained by the evolution of a dark spot on the more massive component. The parabolic variation in the (O - C) curve may be caused by the mass transfer from the massive component to the less massive one in the deep overcontact binary.
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页数:10
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