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WZ CEPHEI: A CLOSE BINARY AT THE BEGINNING OF CONTACT PHASE
Zhu LY(朱俐颖)1,2; Qian SB(钱声帮)1,2; Zhu, LY (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
Source PublicationASTRONOMICAL JOURNAL
2009-12
Volume138Issue:6Pages:2002-2006
DOI10.1088/0004-6256/138/6/2002
Contribution Rank第1完成单位
Indexed BySCI
KeywordBinaries: Close Binaries: Eclipsing Stars: Evolution Stars: Individual (Wz Cephei)
AbstractPhotometric photoelectric data of the short-period close binary system, WZ Cephei, are presented. A new photometric analysis with the 2003 version of the Wilson-Devinney method confirmed that it is a shallow contact binary (f similar to 13.3%) with a high level of spot activity on the primary component. Combining new determined times of light minimum with the others published in the literature, the period change of the binary star is investigated. A periodic variation, with a period of 34.2 years and an amplitude of 0(d).013, was discovered to be superimposed on a long-term period decrease (dP/dt = -8.8 x 10(-8) days year(-1)). Both the secular period decrease and the shallow contact configuration suggest that this binary system is at the beginning of contact phase. It is on the way to evolving into a normal overcontact phase via secular angular momentum loss and/or mass transfer from the more massive component to the less massive one. The period oscillation can be explained either by the light-time effect due to the presence of a third body or by magnetic activity. On the one hand, if it is caused by the light-time effect, the mass and the orbital radius of the additional body should be m(3) = 0.17 M(circle dot) and a(3) = 26.6 AU, respectively, when this body is coplanar to the orbit of the eclipsing pair. On the other hand, since the system shows high levels of spot activity, the period oscillation may be explained as a consequence of magnetic cycles. In this case, the required variation of the quadrupole moment is calculated to be 9.2 x 10(49) g cm(2).
Funding OrganizationThe Chinese Academy of Sciences ; Yunnan Natural Science Foundation [2008CD157] ; National Key Fundamental Research Project [2007CB815406]
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN0004-6256
URL查看原文
Archive Date2009-11-20
WOS IDWOS:000271630200036
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordORBITAL PERIOD MODULATION ; TERM STARSPOT EVOLUTION ; ACTIVITY CYCLE ; LIGHT CURVES ; PHOTOMETRIC MEASUREMENTS ; OVERCONTACT PHASE ; AR LACERTAE ; MASS ; CASSIOPEIAE ; PERSEI
Citation statistics
Cited Times:13[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/5816
Collection双星与变星研究组
Corresponding AuthorZhu, LY (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
Affiliation1.National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China
2.Laboratory for the Structure and Evolution of Celestial Bodies, Chinese Academy of Sciences P.O. Box 110, 650011 Kunming, China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Zhu LY,Qian SB,Zhu, LY . WZ CEPHEI: A CLOSE BINARY AT THE BEGINNING OF CONTACT PHASE[J]. ASTRONOMICAL JOURNAL,2009,138(6):2002-2006.
APA Zhu LY,Qian SB,&Zhu, LY .(2009).WZ CEPHEI: A CLOSE BINARY AT THE BEGINNING OF CONTACT PHASE.ASTRONOMICAL JOURNAL,138(6),2002-2006.
MLA Zhu LY,et al."WZ CEPHEI: A CLOSE BINARY AT THE BEGINNING OF CONTACT PHASE".ASTRONOMICAL JOURNAL 138.6(2009):2002-2006.
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