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Confirmation and revision on the orbital period change of the possible type la supernova progenitor V617 Sagittarii
Shi G(时光)1,2,3; Qian SB(钱声帮)1,2,3; Lajus, EF4,5
Source PublicationPUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
2014-02
Volume66Issue:1Pages:1-6
DOI10.1093/pasj/pst009
Contribution Rank第1完成单位
Indexed BySCI
Keywordbinaries: close binaries: eclipsing stars: evolution stars: individual (V617 Sgr) stars: winds, outflows
Abstract

This work reports new photometric results of eclipsing cataclysmic variable V617 Sagittarii (V617 Sgr). We analyzed the orbital period change of V617 Sgr by employing three new (since 2010) CCD eclipse timings along with all the available data from the literature. It was found that the orbital period of V617 Sgr undergoes an obvious long-term increase, which confirms the result revealed by Steiner et al. (2006). The rate of orbital period increase was calculated to be <(P)over dot> = +2.14(0.05) x 10(-7) d yr(-1). This suggests the lifetime of the secondary star will end in a timescale of 0.97 x 10(6) yr faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 yr and an amplitude of 2.3 min may appear in the O - C diagram. Dominated by the wind-accretion mechanism, high mass transfer from the low mass secondary to the white dwarf is expected to continue in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate vertical bar<(M)over dot>(tr)vertical bar was estimated to be in the range of about 2.2 x 10(-7) to 5.2 x 10(-7) M-circle dot yr(-1). Accordingly, the already massive (>= 1.2 M-circle dot) white dwarf primary will process stable nuclear burning, accrete a fraction of the mass from its companion to reach the standard Chandrasekhar mass limit (similar or equal to 1.38 M-circle dot), and ultimately produce a type la supernova (SN la) within about 4-8 x 10(5) yr or earlier.

Funding ProjectChinese Natural Science Foundation through a key project[11133007]
Funding OrganizationChinese Natural Science Foundation through a key project[11133007]
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星物理学 ; 恒星形成与演化
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherOXFORD UNIV PRESS
Publication PlaceGREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0004-6264
URL查看原文
Archive Date2014-06-09
WOS IDWOS:000339426900009
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordWIND-DRIVEN EVOLUTION ; ASSISTED STELLAR SUICIDE ; X-RAY SOURCES ; V-SAGITTAE ; MAGNETIC BRAKING ; IA SUPERNOVA ; DWARF ; BINARIES ; STARS
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/5905
Collection双星与变星研究组
Corresponding AuthorShi G(时光)
Affiliation1.National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China
2.Yunnan Astronomical Observatory, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, China
3.University of the Chinese Academy of Sciences, Beijing 100049, China
4.Facultad de Ciencias Astrónmicas y Geofisicas, Universidad Nacional de La Plata Paseo del Bosque s/n, 1900, La Plata, Pcia. Bs. As., Argentina
5.Instituto de Astrofisica de La Plata (CCT La plata—CONICET/UNLP), Paseo del Bosque s/n - La Plata, Argentina
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Shi G,Qian SB,Lajus, EF. Confirmation and revision on the orbital period change of the possible type la supernova progenitor V617 Sagittarii[J]. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,2014,66(1):1-6.
APA Shi G,Qian SB,&Lajus, EF.(2014).Confirmation and revision on the orbital period change of the possible type la supernova progenitor V617 Sagittarii.PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,66(1),1-6.
MLA Shi G,et al."Confirmation and revision on the orbital period change of the possible type la supernova progenitor V617 Sagittarii".PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 66.1(2014):1-6.
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