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DEEP, LOW MASS RATIO OVERCONTACT BINARY SYSTEMS. XI. V1191 CYGNI
Zhu LY(朱俐颖)1,2; Qian SB(钱声帮)1,2; Soonthornthum, B3; He JJ(何家佳)1,2; Liu L(刘亮)1,2; Zhu, LY (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Kunming 650011, Peoples R China.
发表期刊ASTRONOMICAL JOURNAL
2011-10
卷号142期号:4
DOI10.1088/0004-6256/142/4/124
产权排序第1完成单位
收录类别SCI
关键词Binaries: Close Binaries: Eclipsing Stars: Evolution Stars: Individual (V1191 Cygni)
摘要Complete CCD photometric light curves in BV(RI)(c) bands obtained on one night in 2009 for the short-period closebinary system V1191 Cygni are presented. A new photometric analysis with the 2003 version of the Wilson-Van Hamme code shows that V1191 Cyg is a W-type overcontact binary system and suggests that it has a high degree of overcontact (f = 68.6%) with very low mass ratio, implying that it is at the late stage of overcontact evolution. The absolute parameters of V1191 Cyg are derived using spectroscopic and photometric solutions. Combining new determined times of light minimum with others published in the literature, the period change of the binary star is investigated. A periodic variation, with a period of 26.7 years and an amplitude of 0.023 days, was discovered to be superimposed on a long-term period increase (dP/dt = +4.5(+/- 0.1) x 10(-7) days yr(-1)). The cyclic period oscillation may be caused by the magnetic activity cycles of either of the components or the light-time effect due to the presence of a third body with a mass of m(3) = 0.77 M-circle dot and an orbital radius of a(3) = 7.6 AU, when this body is coplanar to the orbit of the eclipsing pair. The secular orbital period increase can be interpreted as a mass transfer from the less massive component to the more massive one. With the period increases, V1191 Cyg will evolve from its present low mass ratio, high filled overcontact state to a rapidly rotating single star when its orbital angular momentum is less than three times the total spin angular momentum. V1191 Cyg is too blue for its orbital period and it is an unusual W-type overcontact system with such a low mass ratio and high fill-out overcontact configuration, which is worth monitoring continuously in the future.
项目资助者Special Foundation of the Chinese Academy of Sciences ; West Light Foundation of the Chinese Academy of Science ; Chinese Natural Science Foundation [10973037, 10903026, 11133007] ; Yunnan Natural Science Foundation [2008CD157] ; National Key Fundamental Research Project [2007CB815406]
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-6256
URL查看原文
归档日期2011-11-15
WOS记录号WOS:000295042500028
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]CLOSE-BINARY ; STAR LIGHT ; CONTACT BINARIES ; CURVES ; VELOCITY
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/5851
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Zhu, LY (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Kunming 650011, Peoples R China.
作者单位1.National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, 650011 Kunming, China
2.Key Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences, 650011 Kunming, China
3.National Astronomical Research Institute of Thailand/Ministry of Science and Technology, Bangkok, Thailand
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Zhu LY,Qian SB,Soonthornthum, B,et al. DEEP, LOW MASS RATIO OVERCONTACT BINARY SYSTEMS. XI. V1191 CYGNI[J]. ASTRONOMICAL JOURNAL,2011,142(4).
APA Zhu LY,Qian SB,Soonthornthum, B,He JJ,Liu L,&Zhu, LY .(2011).DEEP, LOW MASS RATIO OVERCONTACT BINARY SYSTEMS. XI. V1191 CYGNI.ASTRONOMICAL JOURNAL,142(4).
MLA Zhu LY,et al."DEEP, LOW MASS RATIO OVERCONTACT BINARY SYSTEMS. XI. V1191 CYGNI".ASTRONOMICAL JOURNAL 142.4(2011).
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