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A Detached Eclipsing Binary with a Period Shorter than 0.2 Days in a Triple System
Zhang, Bin1,2; Qian SB(钱声帮)1,2,3,4,5; Zhi, Q.-J.1,2; Liu NP(刘念平)3,4,5; Dong, A.-J.1,2; Michel, R.6; Zhu LY(朱俐颖)3,4,5; Li, K.7; Zhang J(张嘉)3,4,5; Wang QS(王琪善)3,4,5
Source PublicationPUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
2019-03-01
Volume131Issue:997Pages:13
DOI10.1088/1538-3873/aafeab
Contribution Rank第3完成单位
Indexed BySCI
Keywordstars: activity (stars:) binaries (including multiple): close (stars:) binaries: eclipsing stars: evolution stars: formation stars: fundamental parameters stars: late-type stars: low-mass (stars:) starspots
Abstract

W UMa-type binary stars have an apparent short-period cutoff around 0.2 days. Close binaries with orbital periods shorter than this limit are very useful for understanding the formation and evolution of this type of binaries. 2MASS J11553339+3544399 (hereafter J1155) is a red-dwarf binary with a period of 0.199724 days. Multicolor (V, R, R-c, I, I-c, W) light curves (LCs) for the ultrashort-period eclipsing binary (EB) J1155 are presented and analyzed by using the Wilson-Devinney (W-D) code. We find that J1155 belongs to a rare group of detached red-dwarf EB with periods below the period limit of contact binaries (the other two are BW03 V38 and GSC 2314-0530). It has a high-mass ratio of 0.90. The primary component (the more massive and hotter star) is filling 90% of the critical Roche lobe, while the secondary one is filling about 84.8%. The masses and radii of the two components are estimated as M-1 = 0.475 +/- 0.035 M-circle dot, M-2 = 0.441 +/- 0.044 M-circle dot, R-1 = 0.516 +/- 0.089 R-circle dot, and R-2 = 0.491 +/- 0.105 R-circle dot, respectively. By analyzing all available times of light minimum, the orbital period changes of the binary system are investigated for the first time. We find that the (O - C) (observed-calculated) diagram shows a cyclic oscillation with an amplitude of 0.00326 days and a period about 9.84 years. This oscillation is explained as the light-travel time effect (LTTE) via the presence of a third body. The mass of the third component in the triple system is computed to be M-3 sin (i') similar to 0.127 M-circle dot. The orbital distance between the central binary and the tertiary component is about 4.0 au. It is possible that the third body and the magnetic braking may play important roles in the formation and evolution of J1155 by drawing angular momentum from the central system.

Funding ProjectChinese Natural Science Foundation[11611530685] ; Chinese Natural Science Foundation[11573063] ; Chinese Natural Science Foundation[11503077] ; Chinese Natural Science Foundation[11565010] ; Chinese Natural Science Foundation[U1731238] ; Chinese Natural Science Foundation[U1831120] ; Key Science Foundation of Yunnan Province[2017FA001] ; Guizhou Provincial Joint Fund[20177349] ; Doctor Starting Up Foundation of Guizhou Normal University[0516134] ; National Natural Science Foundation of China (NSFC)[U1631108] ; Chinese Academy of Sciences (CAS)[U1631108] ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
Funding OrganizationChinese Natural Science Foundation[11611530685, 11573063, 11503077, 11565010, U1731238, U1831120] ; Key Science Foundation of Yunnan Province[2017FA001] ; Guizhou Provincial Joint Fund[20177349] ; Doctor Starting Up Foundation of Guizhou Normal University[0516134] ; National Natural Science Foundation of China (NSFC)[U1631108] ; Chinese Academy of Sciences (CAS)[U1631108] ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星天文学 ; 恒星形成与演化
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-6280
URL查看原文
WOS IDWOS:000460822200001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordCLOSE BINARIES ; LIGHT CURVES ; LIMIT
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/19361
Collection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
Corresponding AuthorZhang, Bin
Affiliation1.School of Physics and Electronic Science, Guizhou Normal University, 550001 Guiyang, People's Republic of China
2.Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing, Guizhou Normal University, Guiyang 550001, People's Republic of China
3.Yunnan Observatories, Chinese Academy of Sciences (CAS), P.O. Box 110, 650216 Kunming, People's Republic of China
4.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, P.O. Box 110, Kunming 650216, People's Republic of China
5.University of Chinese Academy of Sciences, Yuquan Road 19#, Sijingshang Block, 100049 Beijing, People's Republic of China
6.Instituto de Astronomía, UNAM, Ensenada, México
7.Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai, 264209, People's Republic of China
Recommended Citation
GB/T 7714
Zhang, Bin,Qian SB,Zhi, Q.-J.,et al. A Detached Eclipsing Binary with a Period Shorter than 0.2 Days in a Triple System[J]. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC,2019,131(997):13.
APA Zhang, Bin.,Qian SB.,Zhi, Q.-J..,Liu NP.,Dong, A.-J..,...&Wang QS.(2019).A Detached Eclipsing Binary with a Period Shorter than 0.2 Days in a Triple System.PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC,131(997),13.
MLA Zhang, Bin,et al."A Detached Eclipsing Binary with a Period Shorter than 0.2 Days in a Triple System".PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC 131.997(2019):13.
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