A New Route to Massive Hot Subdwarfs: Common Envelope Ejection from Asymptotic Giant Branch Stars

doi:10.3847/1538-4357/ad2206

YNAO OpenIR > 大样本恒星演化研究组

	A New Route to Massive Hot Subdwarfs: Common Envelope Ejection from Asymptotic Giant Branch Stars
	Li ZW(李振威)1,2,3 ; Zhang, Yangyang 4; Chen HL(陈海亮)1,2,3 ; Ge HW(葛宏伟)1,2,3 ; Jiang DK(姜登凯)1,2,3 ; Li JD(李江丹)1,2,3 ; Chen XF(陈雪飞)1,2,3 ; Han ZW(韩占文)1,2,3,5
发表期刊	ASTROPHYSICAL JOURNAL
	2024-03-01
卷号	964 期号:1
DOI	10.3847/1538-4357/ad2206
产权排序	第1完成单位
收录类别	SCI
摘要	The hot subdwarf O/B stars (sdO/Bs) are known as extreme horizontal branch stars, which is of great importance in stellar evolution theory. The sdO/Bs are generally thought to have a helium-burning core and a thin hydrogen envelope (M env < 0.02 M (circle star)). In the canonical binary evolution scenario, sdO/Bs are considered to be the stripped cores of red giants. However, such a scenario cannot explain the recently discovered sdO/B binary SMSS J1920, where the strong Ca H and K lines in the spectrum are found. It suggests that this binary likely originated from the recent ejection of the common envelope (CE). In this work, we propose a new formation channel of massive sdO/Bs, namely, sdO/Bs produced from a CE ejection process with an asymptotic giant branch (AGB) star (hereafter the AGB CE channel). We constructed the evolutionary model of sdO/Bs and successfully explained most of the important observed parameters of the sdO/B star in SMSS J1920, including the evolutionary age, sdO/B mass, effective temperature, surface gravity, and surface helium abundance. The minimum sdO/B mass produced from the AGB CE channel is about 0.48 M-circle star. The evolutionary tracks in the logTeff-logg plane may explain a fraction of the observational samples with high logTeff and low logg . Considering the wind mass loss of sdO/Bs, the model could produce helium-rich hot subdwarfs with log(nHe/nH)greater than or similar to-1 .
资助项目	MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[12125303]; MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[12288102]; MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[12090040/3]; MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[11733008]; MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[12103086]; MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[11703081]; MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[11422324]; MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[12073070]; Natural Science Foundation of China[2021YFA1600403]; Natural Science Foundation of China[2021YFA1600400]; Natural Science Foundation of China[202305AB350003]; National Key R&D Program of China[2018076]; Youth Innovation Promotion Association of the Chinese Academy of Sciences[ZDBS-LY-7005]; Key Research Program of Frontier Sciences of CAS[202301AT070314]; Key Research Program of Frontier Sciences of CAS[202101AU070276]; Key Research Program of Frontier Sciences of CAS[202101AV070001]; Yunnan Fundamental Research Projects[202302AN360001]; International Centre of Supernovae, Yunnan Key Laboratory[CMS-CSST-2021-A10]; International Centre of Supernovae, Yunnan Key Laboratory[CMS-CSST-2021-A08]; China Manned Space Project; Stellar Astrophysics Group at Yunnan Observatories, Chinese Academy of Sciences
项目资助者	MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166[12125303, 12288102, 12090040/3, 11733008, 12103086, 11703081, 11422324, 12073070] ; Natural Science Foundation of China[2021YFA1600403, 2021YFA1600400, 202305AB350003] ; National Key R&D Program of China[2018076] ; Youth Innovation Promotion Association of the Chinese Academy of Sciences[ZDBS-LY-7005] ; Key Research Program of Frontier Sciences of CAS[202301AT070314, 202101AU070276, 202101AV070001] ; Yunnan Fundamental Research Projects[202302AN360001] ; International Centre of Supernovae, Yunnan Key Laboratory[CMS-CSST-2021-A10, CMS-CSST-2021-A08] ; China Manned Space Project ; Stellar Astrophysics Group at Yunnan Observatories, Chinese Academy of Sciences
语种	英语
学科领域	天文学
文章类型	Article
出版者	IOP Publishing Ltd
出版地	TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN	0004-637X
URL	查看原文
WOS记录号	WOS:001183782700001
WOS研究方向	Astronomy & Astrophysics
WOS类目	Astronomy & Astrophysics
关键词[WOS]	WHITE-DWARF ; B-STARS ; CONVECTIVE BOUNDARIES ; RICH SUBDWARFS ; STELLAR HALO ; ASTROPHYSICS ; BINARIES ; MODULES ; MESA ; EVOLUTION
引用统计
文献类型	期刊论文
版本	出版稿
条目标识符	http://ir.ynao.ac.cn/handle/114a53/26471
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], [email protected]; 2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Science, People's Republic of China; 3.International Centre of Supernovae, Yunnan Key Laboratory, Kunming, 650216, People's Republic of China; 4.Zhoukou Normal University, East Wenchang Street, Chuanhui District, Zhoukou, 466001, People's Republic of China; 5.University of the Chinese Academy of Science, Yuquan Road 19, Shijingshan Block, 100049, Beijing, 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	Li ZW,Zhang, Yangyang,Chen HL,et al. A New Route to Massive Hot Subdwarfs: Common Envelope Ejection from Asymptotic Giant Branch Stars[J]. ASTROPHYSICAL JOURNAL,2024,964(1).
APA	李振威.,Zhang, Yangyang.,陈海亮.,葛宏伟.,姜登凯.,...&韩占文.(2024).A New Route to Massive Hot Subdwarfs: Common Envelope Ejection from Asymptotic Giant Branch Stars.ASTROPHYSICAL JOURNAL,964(1).
MLA	李振威,et al."A New Route to Massive Hot Subdwarfs: Common Envelope Ejection from Asymptotic Giant Branch Stars".ASTROPHYSICAL JOURNAL 964.1(2024).

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