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Hydrogen and helium shell burning during white dwarf accretion
Cui X(崔晓)1,2,3; Meng XC(孟祥存)1,2; Han ZW(韩占文)1,2; Cui X(崔晓), Email: cx@ynao.ac.cn; Han ZW(韩占文), Email: zhanwenhan@ynao.ac.cn
发表期刊RESEARCH IN ASTRONOMY AND ASTROPHYSICS
2018-05-01
卷号18期号:5
DOI10.1088/1674-4527/18/5/58
产权排序第1完成单位
收录类别SCI
关键词Stars: Evolution Supernovae: General White Dwarfs
摘要Type la supernovae (SNe la) are believed to be thermonuclear explosions of carbon oxygen (CO) white dwarfs (WDs) with masses dose to the Chandrasekhar mass limit. How a CO WD accretes matter and grows in mass to this limit is not well understood, hindering our understanding of SN la explosions and the reliability of using SNe la as a cosmological distance indicator. In this work, we employed the stellar' evolution code MESA to simulate the accretion process of hydrogen-rich material onto a 1.0 M-circle dot CO WD at a high rate (over the Eddington limit) of 4.3 x 10(-7) M-circle dot yr(-1). The simulation demonstrates the characteristics of the double shell burning on top of the WD, with a hydrogen shell burning on top of a helium burning shell. The results show that helium shell burning is not steady (i.e. it flashes). Clashes from the helium shell are weaker than those in the case of accretion of helium-rich material onto a CO WD. The carbon to oxygen mass ratio resulting from the helium shell burning is higher than what was previously thought. Interestingly, the CO WD growing due to accretion has an outer part containing a small fraction of helium in addition to carbon and oxygen. The flashes become weaker and weaker as the accretion continues.
项目资助者National Natural Science Foundation of China(11521303, 11733008, 11390374, 11473063, 11522327, 11703081) ; Natural Science Foundation of Yunnan Province(2013HA005, 2017HC018, 2015HB096) ; CAS Light of West China Program ; Chinese Academy of Sciences(KJZD-EW-M06-01)
语种英语
学科领域天文学
文章类型Article
ISSN1674-4527
URL查看原文
WOS记录号WOS:000432273900010
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]MASS ACCUMULATION EFFICIENCY ; SINGLE-DEGENERATE CHANNEL ; IA SUPERNOVAE ; PROGENITORS ; EVOLUTION ; STARS ; MODEL ; BINARIES ; FLASHES ; GIANT
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/12392
专题大样本恒星演化研究组
中国科学院天体结构与演化重点实验室
通讯作者Cui X(崔晓), Email: cx@ynao.ac.cn; Han ZW(韩占文), Email: zhanwenhan@ynao.ac.cn
作者单位1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China
3.University of Chinese Academy of Sciences, Beijing 100049, China
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Cui X,Meng XC,Han ZW,et al. Hydrogen and helium shell burning during white dwarf accretion[J]. RESEARCH IN ASTRONOMY AND ASTROPHYSICS,2018,18(5).
APA Cui X,Meng XC,Han ZW,Cui X,&Han ZW.(2018).Hydrogen and helium shell burning during white dwarf accretion.RESEARCH IN ASTRONOMY AND ASTROPHYSICS,18(5).
MLA Cui X,et al."Hydrogen and helium shell burning during white dwarf accretion".RESEARCH IN ASTRONOMY AND ASTROPHYSICS 18.5(2018).
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