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Am-Type Eclipsing Binary V2787 Ori: An Evolved Shallow-contact Binary with an Extremely Low Mass Ratio
Tian XM(田晓慢)1,2,3; Zhu LY(朱俐颖)1,2,3,4; Wang ZH(王志华)1,2,3
发表期刊PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
2019-08-01
卷号131期号:1002页码:9
DOI10.1088/1538-3873/ab221e
产权排序第1完成单位
收录类别SCI
关键词(stars:) binaries (including multiple): close (stars:) binaries: eclipsing stars: evolution Online material: color figures
摘要

The first complete multicolor CCD light curves and low-resolution spectra of the short-period Am-type eclipsing binary V2787 Ori are presented. The atmospheric parameters of the primary component, including the effective temperature (T), the gravitational acceleration (log g), and the metallicity [Fe/H], are determined as T-eff = 6993 +/- 82 K, log g = 4.10 +/- 0.22 cm/s(2), and [Fe/H] = -0.40 +/- 0.18 dex, respectively. The Wilson-Devinney (W-D) code was used to analyze those BVRcIc light curves, and the photometric solutions of this eclipsing binary were derived for the first time. It was discovered that V2787 Ori is a shallow-contact, total-eclipsing binary with a factor of f = 0.181(+/- 0.077) and an extremely low mass ratio of q = 0.120(+/- 0.002). The primary contributes about 95% luminosity to the total system, and the temperature difference between the two components exceeds 1600 K. This target may be the smallest mass ratio B-subtype system, but it definitely is among the smallest mass ratio B-subtype systems. The temperature of the secondary is determined as 5413 K, while its mass is estimated as M-2 = 0.17(+/- 0.01) M-circle dot. These properties indicate that the binary may undergo a special evolution where the secondary may be the original more massive component and has transferred most of its mass to its companion. We combined our newly determined eclipse times with those collected from the previous literature, and found that the O - C curve of the binary system shows a cyclic variation with an amplitude of 0.0054 days and a period of 17.3 years, which is explained as the result of the light-time effect, due to a third body orbiting around the central binary. The minimal mass of the third body is 0.208 M-circle dot, and the corresponding orbital radius is about 7.24 au. The shallow-contact configuration, the extremely low mass ratio, the evolved components, and the presence of a tertiary component, all make the B-subtype Am-type contact binary a significant target for further investigations.

资助项目National Natural Science Foundation of China[11573063] ; National Natural Science Foundation of China[11611530685] ; Key Science Foundation of Yunnan Province[2017FA001] ; CAS "Light of West China" Program ; CAS Interdisciplinary Innovation Team
项目资助者National Natural Science Foundation of China[11573063, 11611530685] ; Key Science Foundation of Yunnan Province[2017FA001] ; CAS "Light of West China" Program ; CAS Interdisciplinary Innovation Team
语种英语
学科领域天文学 ; 恒星与银河系 ; 恒星天文学 ; 恒星形成与演化
学科门类理学 ; 理学::天文学
文章类型Article
出版者IOP PUBLISHING LTD
出版地TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-6280
URL查看原文
WOS记录号WOS:000475383600001
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]THERMAL RELAXATION OSCILLATION ; PHYSICAL PARAMETERS ; RADIAL-VELOCITY ; PERIOD CHANGES ; MAGNETIC CYCLES ; STARS ; SYSTEMS ; MULTIPLICITY ; PHOTOMETRY ; COMPONENTS
引用统计
被引频次:9[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/20525
专题双星与变星研究组
中国科学院天体结构与演化重点实验室
通讯作者Tian XM(田晓慢)
作者单位1.Yunnan Observatories, Chinese Academy of Sciences (CAS), P.O. Box 110, 650216 Kunming, People's Republic of China
2.Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences, P.O. Box 110, 650216 Kunming, People's Republic of China
3.University of the Chinese Academy of Science Yuquan Road 19, Sijingshang Block, 100049 Beijing, People's Republic of China
4.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China
第一作者单位中国科学院云南天文台
通讯作者单位中国科学院云南天文台
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Tian XM,Zhu LY,Wang ZH. Am-Type Eclipsing Binary V2787 Ori: An Evolved Shallow-contact Binary with an Extremely Low Mass Ratio[J]. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC,2019,131(1002):9.
APA Tian XM,Zhu LY,&Wang ZH.(2019).Am-Type Eclipsing Binary V2787 Ori: An Evolved Shallow-contact Binary with an Extremely Low Mass Ratio.PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC,131(1002),9.
MLA Tian XM,et al."Am-Type Eclipsing Binary V2787 Ori: An Evolved Shallow-contact Binary with an Extremely Low Mass Ratio".PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC 131.1002(2019):9.
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