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Convective Overshooting in sdB Stars Using the k-omega Model
Li Y(李焱)1,2,3,4; Chen XH(陈兴浩)1,2; Xiong HR(熊赫然)1,2; Guo JJ(郭军军)1,4; Chen XF(陈雪飞)1,2,3; Han ZW(韩占文)1,2,3,4
Source PublicationASTROPHYSICAL JOURNAL
2018-08-10
Volume863Issue:1
DOI10.3847/1538-4357/aacdf9
Contribution Rank第1完成单位
Indexed BySCI
KeywordConvection Stars: Evolution Stars: Interiors Subdwarfs
Abstract

Mixing in the convective core is quite uncertain in core helium-burning stars. To explore the overshooting mixing beyond the convective core, we incorporated the k-omega proposed by Li into the Modules of Experiments in Stellar Astrophysics (MESA), and investigated the overshooting mixing in evolution of subdwarf B (sdB) models. We found that the development of the convective core can be divided into three stages. When the radiative temperature gradient, del(rad), monotonically decreases outwardly, the overshooting mixing presents exponential decay similar with Herwig, and the overshooting distance is to make del(rad) similar or equal to del(ad) at the boundary of the convective core, in agreement with the prediction of the self-driving mechanism Castellani et al. When the radiative temperature gradient, del(rad), shows a minimum value near the convective boundary, the convective core may be divided into two if the minimum value of del(rad) is smaller than the adiabatic temperature gradient del(ad). For the single-zone case, the overshooting mixing shows exponential decay, but the overshooting distance is much smaller than in the initial stage. For the double-zone case, the overshooting mixing is similar to that of the single case beyond the convective core, while it almost stops on both sides of the above convective shell. Our overshooting mixing scheme is similar to the maximal overshoot scheme of Constantino et al. In the final stage, helium injections into the convective core by the overshooting mixing happens, similar to the "core breathing pulses."

Funding ProjectNSFC of China[11333006] ; NSFC of China[11733008] ; NSFC of China[11521303] ; Yunnan Province[2017HC018]
Funding OrganizationNSFC of China[11333006, 11733008, 11521303] ; Yunnan Province[2017HC018]
Language英语
Subject Area天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS IDWOS:000440973300012
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordSubdwarf-b-stars ; Horizontal-branch Stars ; Atomic Diffusion ; Evolution ; Origin
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/17391
Collection恒星物理研究组
中国科学院天体结构与演化重点实验室
Corresponding AuthorLi Y(李焱)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People's Republic of China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, People's Republic of China
3.Center for Astronomical Mega-Science, Chinese Academy of Sciences, Beijing 100012, People's Republic of China
4.University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Li Y,Chen XH,Xiong HR,et al. Convective Overshooting in sdB Stars Using the k-omega Model[J]. ASTROPHYSICAL JOURNAL,2018,863(1).
APA Li Y,Chen XH,Xiong HR,Guo JJ,Chen XF,&Han ZW.(2018).Convective Overshooting in sdB Stars Using the k-omega Model.ASTROPHYSICAL JOURNAL,863(1).
MLA Li Y,et al."Convective Overshooting in sdB Stars Using the k-omega Model".ASTROPHYSICAL JOURNAL 863.1(2018).
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