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A low-mass-ratio and deep contact binary as the progenitor of the merger V1309 Sco
Zhu LY(朱俐颖)1,2,3; Zhao EG(赵二刚)1,2,3; Zhou X(周肖)1,2,3
Source PublicationRESEARCH IN ASTRONOMY AND ASTROPHYSICS
2016-04-01
Volume16Issue:4
DOI10.1088/1674-4527/16/4/068
Contribution Rank第1完成单位
Indexed BySCI
KeywordStars: Binaries: Close Stars: Binaries: Eclipsing Stars: Individuals (V1309 Sco) Stars: Evolution Stars: Mass-loss
Abstract

Nova Sco 2008 (=V1309 Sco) is an example of a V838 Mon type eruption rather than a typical classical nova. This enigmatic object was recently shown to have resulted from the merger of two stars in a contact binary. It is the first stellar merger that was identified to be undergoing a common envelope transient. To understand the properties of its binary progenitor, the pre-outburst light curves were analyzed by using the W-D method. The photometric solution of the 2002 light curve shows that it is a deep contact binary (f = 89.5 (+/- 40.5)%) with a mass ratio of 0.094. The asymmetry of the light curve is explained by the presence of a dark spot on the more massive component. The extremely high fill-out factor suggests that the merging of the contact binary is driven by dynamical mass loss from the outer Lagrange point. However, the analysis of the 2004 light curve indicates that no solutions were obtained even at an extremely low mass ratio of q = 0.03. This suggests that the common convective envelope of the binary system disappeared and the secondary component spiraled into the envelope of the primary in 2004. Finally, the ejection of the envelope of the primary produced the outburst.

Funding ProjectNational Natural Science Foundation of China[11133007] ; National Natural Science Foundation of China[11325315] ; National Natural Science Foundation of China[11573063] ; Key Research Program of the Chinese Academy of Sciences[KGZD-EW-603] ; Science Foundation of Yunnan Province[2012HC011] ; Science Foundation of Yunnan Province[2013FB084] ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences[XDB09010202]
Funding OrganizationNational Natural Science Foundation of China[11133007, 11325315, 11573063] ; Key Research Program of the Chinese Academy of Sciences[KGZD-EW-603] ; Science Foundation of Yunnan Province[2012HC011, 2013FB084] ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences[XDB09010202]
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
PublisherNATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
Publication Place20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA
ISSN1674-4527
URL查看原文
Archive Date2016-05-11
WOS IDWOS:000375006700016
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordTHERMAL RELAXATION OSCILLATION ; OVERCONTACT BINARY ; STELLAR MERGER ; CLOSE-BINARY ; LIGHT CURVES ; SYSTEMS ; CANDIDATE ; EVOLUTION ; SCORPII ; MODELS
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/9586
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 AuthorZhu LY(朱俐颖)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China
2.Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China
3.University of the Chinese Academy of Sciences, Beijing 100049, China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Zhu LY,Zhao EG,Zhou X. A low-mass-ratio and deep contact binary as the progenitor of the merger V1309 Sco[J]. RESEARCH IN ASTRONOMY AND ASTROPHYSICS,2016,16(4).
APA Zhu LY,Zhao EG,&Zhou X.(2016).A low-mass-ratio and deep contact binary as the progenitor of the merger V1309 Sco.RESEARCH IN ASTRONOMY AND ASTROPHYSICS,16(4).
MLA Zhu LY,et al."A low-mass-ratio and deep contact binary as the progenitor of the merger V1309 Sco".RESEARCH IN ASTRONOMY AND ASTROPHYSICS 16.4(2016).
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