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The binary fraction of blue horizontal branch stars

文献类型：期刊论文

作者Guo YJ(郭彦君)2,3; Chen K(陈琨)2,3; Li ZW(李振威)2,3; Ju, Jie4,5; Liu, Chao6; Xue, Xiangxiang6; Dorsch, Matti1; Han ZW(韩占文)2,3; Chen XF(陈雪飞)2,3
刊名ASTRONOMY & ASTROPHYSICS
出版日期2025-09-26
卷号702
关键词methods: data analysis methods: statistical catalogs surveys binaries: spectroscopic stars: horizontal-branch
ISSN号0004-6361
DOI10.1051/0004-6361/202555002
产权排序第1完成单位
文献子类Article
英文摘要Context. Blue horizontal branch (BHB) stars are old, low-mass, metal-poor stars that serve as important tracers of the Galactic halo structure, kinematics, and evolution. Understanding their binary properties provides key insights into their formation channels and the role of binary interactions in the evolution of horizontal branch stars. Aims. We investigated the intrinsic binary fraction f(b)(in) of BHB stars and its dependences on metallicity, kinematics, and effective temperature. Methods. We collected 299 BHB stars from LAMOST with multiple radial velocity (RV) measurements and classified the sample into halo-like and disk-like BHBs based on their kinematics and metallicity, and into bluer and redder BHBs based on their effective temperature. We then investigated the observed binary fraction for each group based on the radial velocity variations and applied a set of Monte Carlo simulations, assuming distributions of f(P)proportional to P-pi and f(q)proportional to q(kappa), to correct the observed binary fraction for observational biases and to derive the intrinsic binary fraction. Results. The observed binary fraction of BHB stars is 18%+/- 2% for cases with n >= 2 and 21%+/- 3% for cases with n >= 3, where n represents the number of observation times. After correcting for observational biases, the intrinsic binary fraction increases to 31%+/- 3% for n >= 2 and 32%+/- 3% for n >= 3. A clear contrast is observed between halo-like and disk-like BHB stars, with halo-like BHBs exhibiting a lower intrinsic binary fraction (28%+/- 3% for n >= 2 and 29%+/- 3% for n >= 3) compared to disk-like BHBs (46%+/- 11% and 51%+/- 11%, respectively), indicating different formation pathways. In particular, halo-like BHB stars are more likely to have formed via a single-star evolution channel, whereas disk-like BHB stars may predominantly result from binary evolution processes. Additionally, we find that bluer BHB stars exhibit a significantly higher binary fraction (42%+/- 6% for n >= 2 and 45%+/- 6% for n >= 3) than redder BHB stars (24%+/- 5% and 23%+/- 5%, respectively), which suggests a possible link between binarity and the effective temperature, although more samples are required to confirm this. No correlation is found between pi (kappa) and metallicity or kinematics, nor between pi (kappa) and the effective temperature of BHB stars.
学科主题天文学 ; 恒星与银河系
URL标识查看原文
出版地17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
WOS关键词SUBDWARF-B-STARS ; GLOBULAR-CLUSTERS ; MULTIPLICITY PROPERTIES ; CHEMICAL ABUNDANCES ; GALACTIC HALO ; HOT STARS ; LAMOST ; EVOLUTION ; KINEMATICS ; VELOCITIES
资助项目Natural Science Foundation of China[12288102]; Natural Science Foundation of China[12125303]; Natural Science Foundation of China[12090040/3]; Natural Science Foundation of China[12103064]; Natural Science Foundation of China[12403039]; Natural Science Foundation of China[12373036]; National Key R&D Program of China[2021YFA1600403/1]; National Key R&D Program of China[2021YFA1600400]; Natural science Foundation of Yunnan Province[202201BC070003]; Natural science Foundation of Yunnan Province[202001AW070007]; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]; Yunnan Revitalization Talent Support Program-Science, Technology Champion Project[202305AB350003]; Yunnan Fundamental Research Projects[202501CF070018]
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001582547500005
出版者EDP SCIENCES S A
资助机构Natural Science Foundation of China[12288102, 12125303, 12090040/3, 12103064, 12403039, 12373036] ; National Key R&D Program of China[2021YFA1600403/1, 2021YFA1600400] ; Natural science Foundation of Yunnan Province[202201BC070003, 202001AW070007] ; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001] ; Yunnan Revitalization Talent Support Program-Science, Technology Champion Project[202305AB350003] ; Yunnan Fundamental Research Projects[202501CF070018]
版本出版稿
源URL[http://ir.ynao.ac.cn/handle/114a53/28625]  
专题云南天文台_大样本恒星演化研究组
通讯作者Guo YJ(郭彦君); Chen XF(陈雪飞)
作者单位1.Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476 Potsdam, Germany
2.Yunnan observatories, Chinese Academy of Sciences, PO Box 110 Kunming 650011, China;
3.International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, China;
4.Department of Physics, Hebei Normal University, Shijiazhuang 050024, People’s Republic of China;
5.School of Sciences, Hebei University of Science and Technology, Shijiazhuang 050018, China;
6.CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China;
推荐引用方式
GB/T 7714		 Guo YJ,Chen K,Li ZW,et al. The binary fraction of blue horizontal branch stars[J]. ASTRONOMY & ASTROPHYSICS,2025,702.
APA 郭彦君.,陈琨.,李振威.,Ju, Jie.,Liu, Chao.,...&陈雪飞.(2025).The binary fraction of blue horizontal branch stars.ASTRONOMY & ASTROPHYSICS,702.
MLA 郭彦君,et al."The binary fraction of blue horizontal branch stars".ASTRONOMY & ASTROPHYSICS 702(2025).

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来源：云南天文台

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