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A NEW PHOTOMETRIC INVESTIGATION OF THE W UMA-TYPE BINARY BI CVn
Qian SB(钱声帮)1,2,3; He JJ(何家佳)1,2,3; Liu L(刘亮)1,2,3; Zhu LY(朱俐颖)1,2,3; Liao WP(廖文萍)1,2,3; Qian, SB (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
发表期刊ASTRONOMICAL JOURNAL
2008-12
卷号136期号:6页码:2493-2501
DOI10.1088/0004-6256/136/6/2493
产权排序第1完成单位
收录类别SCI
关键词Binaries: Close Binaries: Eclipsing Stars: Individual (Bi Cvn) Stars: Evolution
摘要New photometric observations and their investigation of the W UMa-type binary, BI CVn, are presented. The variations of the orbital period were analyzed based on 12 new determined times of light minimum together with the others compiled from the literature. It is discovered that the period of BI CVn shows a long-term period decrease at a rate of. (P) over dot = -1.51(+/- 0.12) x 10(-7) days year(-1) while it undergoes a cyclic variation with a period of 27.0 years and an amplitude of 0(d).0151. Photometric solutions determined with the Wilson-Devinney method suggest that BI CVn is a contact binary with a degree of contact of 18.0(+/- 1.7)%. The asymmetry of the light curves was interpreted by the presence of dark spots on both components, and absolute parameters were determined by combining the photometric elements with the spectroscopic solutions given by Lu. The observed period decrease can be plausibly explained by a combination of the mass transfer from the primary to the secondary and angular momentum loss via magnetic braking. The cyclic period oscillation suggests that BI CVn is a triple system containing a tertiary component with a mass no less than 0.58 M(circle dot) in a 27.0 year orbit. As in the cases of the other contact binaries (e. g., AH Cnc, AP Leo, AD Cnc, and UX Eri), it is possible that this tertiary companion played an important role for the formation and evolution of the contact system by removing angular momentum from the central system via Kozai oscillation or a combination of Kozai cycle and tidal friction, which causes the eclipsing pair to have a short initial orbital period (e. g., P < 5(d)). In that case, can the initially detached system evolve into the present contact configuration via a combination of magnetic torques from stellar winds and a case A mass transfer?
项目资助者Yunnan Natural Science Foundation(2005A0059M) ; Chinese Natural Science(10573032, 10433030) ; National Key Fundamental Research Project(2007CB815406) ; Chinese Academy of Sciences(O8ZKY11001)
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2008-11-24
WOS记录号WOS:000261042500023
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]THERMAL RELAXATION OSCILLATION ; ORBITAL PERIOD MODULATION ; URSAE MAJORIS SYSTEMS ; OVERCONTACT BINARIES ; CLOSE BINARIES ; LIGHT CURVES ; MASS-RATIO ; CONTACT ; PARAMETERS ; EVOLUTION
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/5806
专题双星与变星研究组
通讯作者Qian, SB (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
作者单位1.National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences (CAS), P.O. Box 110, 650011 Kunming, People's Republic of China
2.United Laboratory of Optical Astronomy, Chinese Academy of Sciences (ULOAC), 100012 Beijing, People's Republic of China
3.Graduate University of the Chinese Academy of Sciences, 10049 Beijing, People's Republic of China
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Qian SB,He JJ,Liu L,et al. A NEW PHOTOMETRIC INVESTIGATION OF THE W UMA-TYPE BINARY BI CVn[J]. ASTRONOMICAL JOURNAL,2008,136(6):2493-2501.
APA Qian SB,He JJ,Liu L,Zhu LY,Liao WP,&Qian, SB .(2008).A NEW PHOTOMETRIC INVESTIGATION OF THE W UMA-TYPE BINARY BI CVn.ASTRONOMICAL JOURNAL,136(6),2493-2501.
MLA Qian SB,et al."A NEW PHOTOMETRIC INVESTIGATION OF THE W UMA-TYPE BINARY BI CVn".ASTRONOMICAL JOURNAL 136.6(2008):2493-2501.
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