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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.
发表期刊ASTRONOMICAL JOURNAL
2004-11
卷号128期号:5页码:2430-2434
DOI10.1086/425051
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 (Gr Virginis)
摘要Orbital 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.
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2004-12-28
WOS记录号WOS:000224866500034
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]ORBITAL PERIOD MODULATION ; URSAE-MAJORIS ; CLOSE BINARIES ; MASS-RATIO ; AM LEONIS ; STARS ; PHOTOMETRY ; SYSTEM ; BV
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被引频次:52[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/5768
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, P.O. Box 110, 650011 Kunming
2.United Laboratory of Optical Astronomy, Chinese Academy of Sciences, 100012 Beijing, China
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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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