Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars

doi:10.3847/1538-4365/ad6263

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	Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars
	Zhang LF(张力夫)1,2 ; Ge HW(葛宏伟)1,3,4 ; Chen XF(陈雪飞)1,2,3,4 ; Han ZW(韩占文)1,2,3,4
发表期刊	ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
	2024-09-01
卷号	274 期号:1
DOI	10.3847/1538-4365/ad6263
产权排序	第1完成单位
收录类别	SCI
摘要	The unstable mass transfer situation in binary systems will asymptotically cause the adiabatic expansion of the donor star and finally lead to the common envelope phase. This process could happen in helium binary systems once the helium donor star fills its Roche-lobe. We have calculated the adiabatic mass-loss model of naked helium stars with a mass range of 0.35 M-circle dot-10 M-circle dot, and every mass sequence evolved from the helium-zero-age main sequence to the cooling track of white dwarf or carbon ignition. In consideration of the influence of stellar wind, massive helium stars are not considered in this paper. Comparing the stellar radius with the evolution of the Roche-lobe under the assumption of conservative mass transfer, we give the critical mass ratio q(crit) = M-He/M-accretor as the binary stability criteria of low- and intermediate-mass helium binary stars. On the helium main sequence, the result shows 1.0 < q(crit) < 2.6, which is more unstable than the classical result of polytropic model q(crit) = 3. After the early helium Hertzsprung Gap, the q crit quickly increases even larger than 10 (more stable compared with the widely used result of q(crit) = 4), which is dominated by the expansion of the radiative envelope. Our result could be useful for these quick mass transfer binary systems such as AM CVns, ultra-compact X-ray binaries, and helium novae, and it could guide the binary population synthesis for the formation of special objects such as type Ia supernova and gravitational wave sources.
资助项目	National Natural Science Foundation of China (NSFC)[12288102]; National Natural Science Foundation of China (NSFC)[12125303]; National Natural Science Foundation of China (NSFC)[12090040/3]; National Natural Science Foundation of China (NSFC)[12173081]; National Key R&D Program of China[2021YFA1600403]; National Key R&D Program of China[2021YFA1600401]; Key Research Program of Frontier Sciences; CAS, CAS-Light of West China Program, Yunnan Fundamental Research Projects[ZDBS-LY-7005]; Yunnan Fundamental Research Projects[202101AV070001]; Yunnan Fundamental Research Projects[202201BC070003]; Yunnan Fundamental Research Projects[202401BC070007]; Yunnan Revitalization Talent Support Program-Science & Technology Champion Project[202305AB350003]; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]
项目资助者	National Natural Science Foundation of China (NSFC)[12288102, 12125303, 12090040/3, 12173081] ; National Key R&D Program of China[2021YFA1600403, 2021YFA1600401] ; Key Research Program of Frontier Sciences ; CAS, CAS-Light of West China Program, Yunnan Fundamental Research Projects[ZDBS-LY-7005] ; Yunnan Fundamental Research Projects[202101AV070001, 202201BC070003, 202401BC070007] ; Yunnan Revitalization Talent Support Program-Science & Technology Champion Project[202305AB350003] ; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]
语种	英语
学科领域	天文学 ; 恒星与银河系
文章类型	Article
出版者	IOP Publishing Ltd
出版地	TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN	0067-0049
URL	查看原文
WOS记录号	WOS:001308539100001
WOS研究方向	Astronomy & Astrophysics
WOS类目	Astronomy & Astrophysics
关键词[WOS]	STELLAR EVOLUTION MODELS ; SUBDWARF-B-STARS ; STABILITY ; PROGRAM ; RATIO ; IDENTIFICATION ; PROGENITORS ; CRITERIA ; CHANNEL ; ORIGIN
引用统计	被引频次：2[WOS] [WOS记录] [WOS相关记录]
文献类型	期刊论文
版本	出版稿
条目标识符	http://ir.ynao.ac.cn/handle/114a53/27584
专题	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
作者单位	1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People's Republic of China; [email protected]; 2.University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China; 3.Key Laboratory for Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, P.O. Box 110, Kunming 650216, People's Republic of China; 4.International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, People's Republic of China
第一作者单位	中国科学院云南天文台
推荐引用方式 GB/T 7714	Zhang LF,Ge HW,Chen XF,et al. Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2024,274(1).
APA	张力夫,葛宏伟,陈雪飞,&韩占文.(2024).Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars.ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,274(1).
MLA	张力夫,et al."Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars".ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 274.1(2024).

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