| 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 |
| DOI | 10.1086/425051 |
| 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 |
| ISSN | 0004-6256 |
| 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 |
| 引用统计 | |
| 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 |
| 推荐引用方式 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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| GR Virginis_ A Deep （203KB） | 期刊论文 | 作者接受稿 | 开放获取 | CC BY-NC-SA | 浏览 请求全文 | |
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