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BI VULPECULAE: A SIAMESE TWIN WITH TWO VERY SIMILAR COOL STARS IN SHALLOW CONTACT
Qian SB(钱声帮)1,2,3; Liu NP(刘念平)1,2,3; Li K(李凯)4; He JJ(何家佳)1,2; Zhu LY(朱俐颖)1,2,3; Zhao EG(赵二刚)1,2; Wang JJ(王晶晶)1,2,3; Li LJ(李临甲)1,2,3; Jiang LQ(江林巧)1,2,3; Qian, SB (reprint author), Chinese Acad Sci, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
发表期刊ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
2013-11
卷号209期号:1页码:13-20
DOI10.1088/0067-0049/209/1/13
产权排序第1完成单位
收录类别SCI
关键词Binaries: Close Binaries: Eclipsing Stars: Activity Stars: Evolution Stars: Individual (Bi Vul)
摘要BI Vul is a cool eclipsing binary star (Sp. = K3 V) with a short period of 0.2518 days. The first charge-coupled device (CCD) light curves of the binary in the BVRI obtained on 2012 August 21 are presented and are analyzed using the Wilson-Devinney code. It is discovered that BI Vul is a marginal contact binary system (f = 8.7%) that contains two very similar cool components (q = 1.037). Both the marginal contact configuration and the extremely high mass ratio suggest that it is presently evolving into contact with little mass transfer between the components and it is at the beginning stage of contact evolution. By using all available times of minimum light, the variations in the orbital period are investigated for the first time. We find that the observed - calculated (O - C) curve of BI Vul shows a cyclic change with a period of 10.8 yr and an amplitude of 0.0057 days, while it undergoes a downward parabolic variation. The cyclic oscillation is analyzed for the light-travel time effect that arises from the gravitational influence of a possible third stellar object. The mass and orbital separation of the third body are estimated asM(3) similar to 0.30 M-circle dot and similar to 4.9 AU, respectively. The downward parabolic change reveals a long-term period decrease at a rate of (P) over dot = -9.5 x 10(-8) days yr(-1). The period decrease may be caused by angular momentum loss via magnetic stellar wind and/or it is only a part of a long-period (longer than 32 yr) cyclic variation, which may reveal the presence of another stellar companion in a wider orbit. These observational properties indicate that the formation of the Siamese twin is driven by magnetic braking and the third stellar companion should play an important role by removing angular momentum from the central binary.
项目资助者Chinese Natural Science Foundation [11133007, 11203066] ; West Light Foundation of the Chinese Academy of Sciences
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0067-0049
URL查看原文
归档日期2013-11-19
WOS记录号WOS:000326571000013
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]CLOSE BINARY-SYSTEMS ; THERMAL RELAXATION OSCILLATION ; URSAE MAJORIS SYSTEMS ; ANGULAR-MOMENTUM LOSS ; 4-COLOR LIGHT CURVES ; RADIAL-VELOCITY ; PHYSICAL PARAMETERS ; OVERCONTACT BINARIES ; PERIOD CHANGES ; MASS-RATIO
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/5875
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Qian, SB (reprint author), Chinese Acad Sci, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
作者单位1.Yunnan Observatories, Chinese Academy of Sciences (CAS), P. O. Box 110, 650011 Kunming, China
2.Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, P. O. Box 110, 650011 Kunming, China
3.Graduate University of the Chinese Academy of Sciences, Yuquan Road 19#, Sijingshang Block, 100049 Beijing, China
4.School of Space Science and Physics, Shandong University, Weihai, 264209 Weihai, China
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Qian SB,Liu NP,Li K,et al. BI VULPECULAE: A SIAMESE TWIN WITH TWO VERY SIMILAR COOL STARS IN SHALLOW CONTACT[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2013,209(1):13-20.
APA Qian SB.,Liu NP.,Li K.,He JJ.,Zhu LY.,...&Qian, SB .(2013).BI VULPECULAE: A SIAMESE TWIN WITH TWO VERY SIMILAR COOL STARS IN SHALLOW CONTACT.ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,209(1),13-20.
MLA Qian SB,et al."BI VULPECULAE: A SIAMESE TWIN WITH TWO VERY SIMILAR COOL STARS IN SHALLOW CONTACT".ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 209.1(2013):13-20.
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