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A common-envelope wind model for Type Ia supernovae - I. Binary evolution and birth rate
Meng XC(孟祥存)1,2,3; Podsiadlowski, Ph.4
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2017-08-01
Volume469Issue:4Pages:4763-4787
DOI10.1093/mnras/stx1137
Contribution Rank第1完成单位
Indexed BySCI
KeywordBinaries: Close Stars: Evolution Supernovae: General White Dwarfs
Abstract

The single-degenerate (SD) model is one of the principal models for the progenitors of Type Ia supernovae (SNe Ia), but some of the predictions in the most widely studied version of the SD model, i.e. the optically thick wind (OTW) model, have not been confirmed by observations. Here, we propose a new version of the SD model in which a common envelope (CE) is assumed to form when the mass-transfer rate between a carbon-oxygen white dwarf (CO WD) and its companion exceeds a critical accretion rate. The WD may gradually increase its mass at the base of the CE. Due to the large nuclear luminosity for stable hydrogen burning, the CE may expand to giant dimensions and will lose mass from the surface of the CE by a CE wind (CEW). Because of the low CE density, the binary system will avoid a fast spiral-in phase and finally re-emerge from the CE phase. Our model may share the virtues of the OTW model but avoid some of its shortcomings. We performed binary stellar evolution calculations for more than 1100 close WD + MS binaries. Compared with the OTW model, the parameter space for SNe Ia from our CEW model extends to more massive companions and less massive WDs. Correspondingly, the Galactic birth rate from the CEW model is higher than that from the OTWmodel by similar to 30 per cent. Finally, we discuss the uncertainties of the CEW model and the differences between our CEW model and the OTW model.

Funding ProjectNatural Science Foundation of China[11473063] ; Natural Science Foundation of China[11522327] ; CAS[KJZD-EW-M06-01] ; CAS 'Light of West China' Program ; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences
Funding OrganizationNatural Science Foundation of China[11473063, 11522327] ; CAS[KJZD-EW-M06-01] ; CAS 'Light of West China' Program ; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星物理学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherOXFORD UNIV PRESS
Publication PlaceGREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0035-8711
URL查看原文
WOS IDWOS:000406837900073
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordACCRETING WHITE-DWARFS ; X-RAY SOURCES ; SINGLE-DEGENERATE CHANNEL ; NOVA U-SCORPII ; HIGH-RESOLUTION SPECTROSCOPY ; ASYMPTOTIC-GIANT-BRANCH ; HIGH-VELOCITY FEATURES ; FINAL MASS RELATION ; STELLAR EVOLUTION ; COMPANION STARS
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/11882
Collection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
Corresponding AuthorMeng XC(孟祥存)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, 650216 Kunming, PR China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650216 Kunming, PR China
3.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, PR China
4.Department of Astronomy, Oxford University, Oxford OX1 3RH, UK
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Meng XC,Podsiadlowski, Ph.. A common-envelope wind model for Type Ia supernovae - I. Binary evolution and birth rate[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2017,469(4):4763-4787.
APA Meng XC,&Podsiadlowski, Ph..(2017).A common-envelope wind model for Type Ia supernovae - I. Binary evolution and birth rate.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,469(4),4763-4787.
MLA Meng XC,et al."A common-envelope wind model for Type Ia supernovae - I. Binary evolution and birth rate".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 469.4(2017):4763-4787.
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