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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; Shi, G (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, POB 110, Kunming 650011, Peoples R China.
发表期刊PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
2014-02
卷号66期号:1页码:1-6
DOI10.1093/pasj/pst009
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 (V617 Sgr) Stars: Winds Outflows
摘要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.
项目资助者Chinese Natural Science Foundation through a key project [11133007]
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-6264
URL查看原文
归档日期2014-06-09
WOS记录号WOS:000339426900009
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]WIND-DRIVEN EVOLUTION ; ASSISTED STELLAR SUICIDE ; X-RAY SOURCES ; V-SAGITTAE ; MAGNETIC BRAKING ; IA SUPERNOVA ; DWARF ; BINARIES ; STARS
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被引频次:1[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/5905
专题双星与变星研究组
通讯作者Shi, G (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron 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, 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
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Shi G,Qian SB,Lajus, EF,et al. 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,&Shi, G .(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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