Structure of a massive common envelope in the common-envelope wind model for Type Ia supernovae | |
Song R(宋仁)4,5; Meng XC(孟祥存)1,2,4; Podsiadlowski, Philipp3; Cui YZ(崔英朕)4,5 | |
刊名 | ASTRONOMY & ASTROPHYSICS |
2020-01-08 | |
卷号 | 633页码:10 |
关键词 | binaries close stars evolution supernovae general white dwarfs |
ISSN号 | 0004-6361 |
DOI | 10.1051/0004-6361/201936526 |
产权排序 | 第1完成单位 |
文献子类 | Article |
英文摘要 | Context. Although Type Ia supernovae (SNe Ia) are important in many astrophysical fields, the nature of their progenitors is still unclear. A new version of the single-degenerate model has been developed recently, the common-envelope wind (CEW) model, in which the binary is enshrouded in a common envelope (CE) during the main accretion phase. This model is still in development and has a number of open issues, for example what is the exact appearance of such a system during the CE phase? Aims. In this paper we investigate this question for a system with a massive CE. Methods. We use a thermally pulsing asymptotic giant branch (TPAGB) star with a CO core of 0.976 M-circle dot and an envelope of 0.6 M-circle dot to represent the binary system. The effects of the companion's gravity and the rotation of the CE are mimicked by modifying the gravitational constant. The energy input from the friction between the binary and the CE is taken into account by an extra heating source. Results. For a thick envelope, the modified TPAGB star looks similar to a canonical TPAGB star but with a smaller radius, a higher effective temperature, and a higher surface luminosity. This is primarily caused by the effect of the companion's gravity, which is the dominant factor in changing the envelope structure. The mixing length at the position of the companion can be larger than the local radius, implying a breakdown of mixing-length theory and suggesting the need for more turbulence in this region. The modified TPAGB star is more stable than the canonical TPAGB star and the CE density around the companion is significantly higher than that assumed in the original CEW model. Conclusions. Future work will require the modelling of systems with lower envelope masses and the inclusion of hydrodynamical effects during the CE phase. |
学科主题 | 天文学 ; 恒星与银河系 ; 恒星形成与演化 |
URL标识 | 查看原文 |
出版地 | 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE |
资助项目 | NSFC[11973080] ; NSFC[11733008] ; Yunnan Foundation[2015HB096] ; Yunnan Foundation[2017HC018] ; Yunnan Ten Thousand Talents Plan - Young & Elite Talents Project |
WOS关键词 | WHITE-DWARF MODELS ; CIRCUMSTELLAR MATERIAL ; CENTRAL STAR ; EVOLUTION ; PROGENITORS ; BINARIES ; AGB |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | EDP SCIENCES S A |
WOS记录号 | WOS:000506363000004 |
资助机构 | NSFC[11973080, 11733008] ; Yunnan Foundation[2015HB096, 2017HC018] ; Yunnan Ten Thousand Talents Plan - Young & Elite Talents Project |
内容类型 | 期刊论文 |
源URL | [http://ir.ynao.ac.cn/handle/114a53/22020] |
专题 | 云南天文台_大样本恒星演化研究组 |
通讯作者 | Song R(宋仁) |
作者单位 | 1.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650216 Kunming, PR China 2.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, PR China 3.Department of Astronomy, Oxford University, Oxford OX1 3RH, UK 4.National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650216, PR China 5.University of Chinese Academy of Sciences, Beijing 100049, PR China |
推荐引用方式 GB/T 7714 | Song R,Meng XC,Podsiadlowski, Philipp,et al. Structure of a massive common envelope in the common-envelope wind model for Type Ia supernovae[J]. ASTRONOMY & ASTROPHYSICS,2020,633:10. |
APA | Song R,Meng XC,Podsiadlowski, Philipp,&Cui YZ.(2020).Structure of a massive common envelope in the common-envelope wind model for Type Ia supernovae.ASTRONOMY & ASTROPHYSICS,633,10. |
MLA | Song R,et al."Structure of a massive common envelope in the common-envelope wind model for Type Ia supernovae".ASTRONOMY & ASTROPHYSICS 633(2020):10. |
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