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Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae
Wu CY(吴程远)1,2,3,4; Wang B(王博)1,2,3,4; Liu DD(刘栋栋)1,2,3,4; Han ZW(韩占文)1,2,3,4
Source PublicationASTRONOMY & ASTROPHYSICS
2017-08-01
Volume604
DOI10.1051/0004-6361/201630099
Contribution Rank第1完成单位
Indexed BySCI ; EI
KeywordStars: Evolution Binaries (Including Multiple): Close Supernovae: General White Dwarfs
Abstract

Context. Type Ia supernovae (SNe Ia) play a crucial role in studying cosmology and galactic chemical evolution. They are thought to be thermonuclear explosions of carbon-oxygen white dwarfs (CO WDs) when their masses reach the Chandrasekar mass limit in binaries. Previous studies have suggested that He novae may be progenitor candidates of SNe Ia. However, the mass retention efficiencies during He nova outbursts are still uncertain. 

Aims. In this article, we aim to study the mass retention efficiencies of He nova outbursts and to investigate whether SNe Ia can be produced through He nova outbursts. 

Methods. Using the stellar evolution code Modules for Experiments in Stellar Astrophysics, we simulated a series of multicycle He-layer flashes, in which the initial WD masses range from 0.7 to 1.35 M-circle dot with various accretion rates. 

Results. We obtained the mass retention efficiencies of He nova outbursts for various initial WD masses, which can be used in the binary population synthesis studies. In our simulations, He nova outbursts can increase the mass of the WD to the Chandrasekar mass limit and the explosive carbon burning can be triggered in the center of the WD; this suggests that He nova outbursts can produce SNe Ia. Meanwhile, the mass retention efficiencies in the present work are lower than those of previous studies, which leads to a lower birthrates of SNe Ia through the WD + He star channel. Furthermore, we obtained the elemental abundances distribution at the moment of explosive carbon burning, which can be used as the initial input parameters in studying explosion models of SNe Ia.

Funding ProjectNational Basic Research Program of China (973 programme)[2014CB845700] ; National Natural Science Foundation of China[11673059] ; National Natural Science Foundation of China[11521303] ; National Natural Science Foundation of China[11390374] ; National Natural Science Foundation of China[11573016] ; National Natural Science Foundation of China[11573016] ; Chinese Academy of Sciences[KJZD-EW-M06-01] ; Key Research Program of Frontier Science CAS[QYZDB-SSW-SYS001] ; Youth Innovation Promotion Association CAS ; Natural Science Foundation of Yunnan Province[2013HB097] ; Natural Science Foundation of Yunnan Province[2013HA005]
Funding OrganizationNational Basic Research Program of China (973 programme)[2014CB845700] ; National Natural Science Foundation of China[11673059, 11521303, 11390374, 11573016, 11547041] ; Chinese Academy of Sciences[KJZD-EW-M06-01] ; Key Research Program of Frontier Science CAS[QYZDB-SSW-SYS001] ; Youth Innovation Promotion Association CAS ; Natural Science Foundation of Yunnan Province[2013HB097, 2013HA005]
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
PublisherEDP SCIENCES S A
Publication Place17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
ISSN0004-6361
URL查看原文
WOS IDWOS:000408480100038
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordSINGLE-DEGENERATE CHANNEL ; EDDINGTON WIND SCENARIO ; AM CVN STARS ; LIGHT CURVES ; HELIUM NOVA ; SHELL SOURCE ; DELAY TIMES ; PROGENITORS ; EVOLUTION ; BINARIES
EI Accession Number20173104010065
EI KeywordsWhite dwarfs
EI Classification Number657.2Extraterrestrial Physics and Stellar Phenomena - 804Chemical Products Generally - 913.1Production Engineering
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/10164
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 AuthorWu CY(吴程远)
Affiliation1.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
4.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing; 100012, China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Wu CY,Wang B,Liu DD,et al. Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae[J]. ASTRONOMY & ASTROPHYSICS,2017,604.
APA Wu CY,Wang B,Liu DD,&Han ZW.(2017).Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae.ASTRONOMY & ASTROPHYSICS,604.
MLA Wu CY,et al."Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae".ASTRONOMY & ASTROPHYSICS 604(2017).
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