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Adiabatic Mass Loss in Binary Stars. III. From the Base of the Red Giant Branch to the Tip of the Asymptotic Giant Branch
Ge HW(葛宏伟)1,2,3,4; Webbink, Ronald F.5; Chen XF(陈雪飞)1,2,3,4; Han ZW(韩占文)1,2,3,4
Source PublicationASTROPHYSICAL JOURNAL
2020-08-01
Volume899Issue:2Pages:15
DOI10.3847/1538-4357/aba7b7
Contribution Rank第1完成单位
Indexed BySCI
KeywordStellar evolution Stellar mass loss Close binary stars Common envelope evolution Stellar interiors
Abstract

The distinguishing feature of the evolution of close binary stars is the role played by the mass exchange between the component stars. Whether or not the mass transfer is dynamically stable is one of the essential questions in binary evolution. In the limit of extremely rapid mass transfer, the response of a donor star in an interacting binary becomes asymptotically one of adiabatic expansion. We use the adiabatic mass-loss model to systematically survey the thresholds for dynamical timescale mass transfer over the entire span of possible donor star evolutionary states. We also simulate mass-loss process with isentropic envelopes, the specific entropy of which is fixed to be that at the base of the convective envelope, to artificially mimic the effect of such mass loss in superadiabatic surface convection regions, where the adiabatic approximation fails. We illustrate the general adiabatic response of 3.2 M-circle dot donor stars at different evolutionary stages. We extend our study to a grid of donor stars with different masses (from 0.1 to 100 M-circle dot with Z = 0.02) and at different evolutionary stages. We proceed to present our criteria for dynamically unstable mass transfer in both tabular and graphical forms. For red giant branch (RGB) and asymptotic giant branch (AGB) donors in systems with such mass ratios, they may have convective envelopes deep enough to evolve into common envelopes on a thermal timescale, if the donor star overfills its outer Lagrangian radius. Our results show that the RGB and AGB stars tend to be more stable than previously believed, and this may be helpful to explain the abundance of observed post-AGB binary stars with an orbital period of around 1000 days.

Funding ProjectNational Natural Science Foundation of China (NSFC)[11673058] ; National Natural Science Foundation of China (NSFC)[11733008] ; key research program of frontier sciences, CAS[ZDBSLY-7005] ; Natural Science Foundation of Yunnan Province[2019HA012] ; Department of Astronomy at the University of Illinois at Urbana-Champaign ; US National Science Foundation[AST 04-06726] ; US National Science Foundation[AST 14-13367]
Funding OrganizationNational Natural Science Foundation of China (NSFC)[11673058, 11733008] ; key research program of frontier sciences, CAS[ZDBSLY-7005] ; Natural Science Foundation of Yunnan Province[2019HA012] ; Department of Astronomy at the University of Illinois at Urbana-Champaign ; US National Science Foundation[AST 04-06726, AST 14-13367]
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星物理学 ; 恒星形成与演化
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:000565624100001
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
Citation statistics
Cited Times:2[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/23695
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 AuthorGe HW(葛宏伟)
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, Kunming 650216, 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
5.University of Illinois at Urbana-Champaign, 1002 W Green Street, Urbana, IL 61801, USA
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Ge HW,Webbink, Ronald F.,Chen XF,et al. Adiabatic Mass Loss in Binary Stars. III. From the Base of the Red Giant Branch to the Tip of the Asymptotic Giant Branch[J]. ASTROPHYSICAL JOURNAL,2020,899(2):15.
APA Ge HW,Webbink, Ronald F.,Chen XF,&Han ZW.(2020).Adiabatic Mass Loss in Binary Stars. III. From the Base of the Red Giant Branch to the Tip of the Asymptotic Giant Branch.ASTROPHYSICAL JOURNAL,899(2),15.
MLA Ge HW,et al."Adiabatic Mass Loss in Binary Stars. III. From the Base of the Red Giant Branch to the Tip of the Asymptotic Giant Branch".ASTROPHYSICAL JOURNAL 899.2(2020):15.
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