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GR Virginis: A deep overcontact binary
Qian SB(钱声帮)1,2; Yang YG(杨远贵)1,2; Qian, SB (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
Source PublicationASTRONOMICAL JOURNAL
2004-11
Volume128Issue:5Pages:2430-2434
DOI10.1086/425051
Contribution Rank第1完成单位
Indexed BySCI
KeywordBinaries : Close Binaries : Eclipsing Stars : Evolution Stars : Individual (Gr Virginis)
AbstractOrbital period variations of the low-mass ratio (q = 0.122) overcontact binary system, GR Vir, were investigated by using two new CCD times of minimum light and other photoelectric data compiled from literatures. It is found that the O-C residuals of GR Vir show a cyclic variation with a period of 19.3 yr and an amplitude of 0.0140 days while they are undergoing a long-term decrease (dP/dt = 4.32 x 10(-7) days yr(-1)). Meanwhile, the 1988 photoelectric observations from Cereda et al. were analyzed using the Wilson-Devinney method. Like some low-mass ratio overcontact binary stars (e.g., AW UMa), GR Vir is an A-type overcontact binary with a high degree of overcontact (f = 78.6%). By combining the spectroscopic solutions with the photometric elements, the absolute parameters of the system are determined as follows: M-1 = 1.36 M-circle dot, M-2 = 0.17 M-circle dot, a = 2.40 R-circle dot, R-1 = 1.42 R-circle dot, R-2 = 0.61 R-circle dot, L-1 = 2.87 L-circle dot, and L-2 = 0.48 L-circle dot. The long-term period decrease is interpreted as the result of mass transfer from the more massive component to the less massive one in combination with the angular momentum loss due to mass outflow from the L-2 point. The conditions in GR Vir resemble those in AW UMa. Both systems show a high degree of overcontact, low mass ratios, and secular shrinking of their orbits. As their orbital periods decrease, the shrinking of the inner and outer critical Roche lobes will cause the common convective envelope to become deeper, until finally the formation of single, rapid-rotation stars is inevitable. The period oscillation may by caused either by the presence of an unseen tertiary component (e.g., a white dwarf) or by magnetic activity on the part of the primary component.
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN0004-6256
URL查看原文
Archive Date2004-12-28
WOS IDWOS:000224866500034
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordORBITAL PERIOD MODULATION ; URSAE-MAJORIS ; CLOSE BINARIES ; MASS-RATIO ; AM LEONIS ; STARS ; PHOTOMETRY ; SYSTEM ; BV
Citation statistics
Cited Times:52[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/5768
Collection双星与变星研究组
Corresponding AuthorQian, SB (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
2.United Laboratory of Optical Astronomy, Chinese Academy of Sciences, 100012 Beijing, China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Qian SB,Yang YG,Qian, SB . GR Virginis: A deep overcontact binary[J]. ASTRONOMICAL JOURNAL,2004,128(5):2430-2434.
APA Qian SB,Yang YG,&Qian, SB .(2004).GR Virginis: A deep overcontact binary.ASTRONOMICAL JOURNAL,128(5),2430-2434.
MLA Qian SB,et al."GR Virginis: A deep overcontact binary".ASTRONOMICAL JOURNAL 128.5(2004):2430-2434.
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