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The most plausible explanation of the cyclic period changes in close binaries: the case of the RS CVn-type binary WW Dra
Liao WP(廖文萍)1,2,3; Qian SB(钱声帮)1,2,3; Liao, WP (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, POB 110, Kunming 650011, Peoples R China.
发表期刊MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2010-07-01
卷号405期号:3页码:1930-1939
DOI10.1111/j.1365-2966.2010.16584.x
产权排序第1完成单位
收录类别SCI
关键词Methods: Statistical Binaries: Close Binaries: Eclipsing Stars: Individual: Ww Dra Stars: Late-type
摘要Cyclic period changes are a fairly common phenomenon in close binary systems and are usually explained as being caused either by the magnetic activity of one or both components or by the light travel time effect (LTTE) of a third body. We searched the orbital period changes in 182 EA-type (including the 101 Algol systems used by Hall), 43 EB-type and 53 EW-type binaries with known mass ratio and spectral type of the secondary component. We reproduced and improved the diagram in Hall according to the new collected data. Our plots do not support the conclusion derived by Hall that cyclic period changes are restricted to binaries having a secondary component with spectral type later than F5. The presence of period changes among systems with a secondary component of early type indicates that magnetic activity is one, but not the only, cause of the period variation. It is discovered that cyclic period changes, probably resulting from the presence of a third body, are more frequent in EW-type binaries among close systems. Therefore, the most plausible explanation of the cyclic period changes is the LTTE through the presence of a third body. Using the century-long historical record of the times of light minimum, we analysed the cyclic period change in the Algol binary WW Dra. It is found that the orbital period of the binary shows a similar to 112.2-yr cyclic variation with an amplitude of similar to 0.1977 d. The cyclic oscillation can be attributed to the LTTE by means of a third body with a mass no less than 6.43M(circle dot). However, no spectral lines of the third body were discovered, indicating that it may be a candidate black hole. The third body is orbiting the binary at a distance closer than 14.4 au and may play an important role in the evolution of this system.
项目资助者Chinese Natural Science Foundation [10973037, 10903026, 10778718] ; National Key Fundamental Research Project [2007CB815406] ; Yunnan Natural Science Foundation [2008CD157]
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0035-8711
URL查看原文
归档日期2010-07-09
WOS记录号WOS:000279022900038
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]UNSOLVED QUADRUPLE SYSTEM ; ANGULAR-MOMENTUM LOSS ; NEAR-CONTACT BINARY ; ALGOL-TYPE BINARIES ; ORBITAL PERIOD ; ECLIPSING BINARY ; OVERCONTACT BINARY ; RADIAL-VELOCITY ; TRIPLE SYSTEM ; PHOTOMETRIC ANALYSIS
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/5838
专题双星与变星研究组
中国科学院天体结构与演化重点实验室
通讯作者Liao, WP (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, PO Box 110, 650011 Kunming, China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Yunnan Observatory, PO Box 110, 650011 Kunming, China
3.Graduate School of the CAS, 100049, Beijing, China/Yuquan Road 19#, SijingShan Block, 100049, Beijing City, China
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Liao WP,Qian SB,Liao, WP . The most plausible explanation of the cyclic period changes in close binaries: the case of the RS CVn-type binary WW Dra[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2010,405(3):1930-1939.
APA Liao WP,Qian SB,&Liao, WP .(2010).The most plausible explanation of the cyclic period changes in close binaries: the case of the RS CVn-type binary WW Dra.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,405(3),1930-1939.
MLA Liao WP,et al."The most plausible explanation of the cyclic period changes in close binaries: the case of the RS CVn-type binary WW Dra".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 405.3(2010):1930-1939.
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