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Radial velocity variability fractions of different types of hot subdwarf stars

文献类型：期刊论文

作者He RJ(贺锐杰)5,6; Meng XC(孟祥存)2,5,7; Lei, Zhenxin1,3; Yan, Huahui4; Lan SY(兰顺义)5,6
刊名ASTRONOMY & ASTROPHYSICS
出版日期2025-01-09
卷号693
关键词binaries: close stars: evolution subdwarfs
ISSN号0004-6361
DOI10.1051/0004-6361/202451411
产权排序第1完成单位
文献子类Article
英文摘要Context. It is generally thought that hot subdwarfs are helium-core- or helium-shell-burning objects with extremely thin hydrogen envelopes and that binary interactions are always needed in their formation. Different types of hot subdwarfs may have different origins, which will cause them to present different radial velocity (RV) variability properties. Aims. We plan to study the RV-variability fractions of different types of hot subdwarfs, as well as their distributions in the T-eff - log g diagram. This provides insights into the formation of hot subdwarfs. Methods. The cross-correlation function method was adopted to measure RV variations in 434 hot subdwarfs based on spectra obtained with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST). Light curves from the Transiting Exoplanet Survey were also used to search for short-period binary hot subdwarfs. Results. Only 6 +/- 4% of our single-lined He-rich hot subdwarfs that only show spectroscopic features of hot subdwarfs are found to be RV variable, which is lower than the fraction of single-lined He-poor sdB stars (31 +/- 3%). Single-lined sdB stars with effective temperatures (T-eff) similar to 25 000-33 000 K show an RV-variability fraction of 34 +/- 5%, while lower RV-variability fractions are observed for single-lined sdB stars cooler than about 25 000 K (11 +/- 4%), single-lined sdB/OB stars with T-eff similar to 33 000-40 000 K and surface gravities similar to 5.7-6.0 (13 +/- 3%), as well as single-lined sdO/B stars with T-eff similar to 45 000-70 000 K (10 +/- 7%). Single-lined hot subdwarfs with T-eff similar to 35 000-45 000 K located above the extreme horizontal branch (EHB) show a similar RV-variability fraction of 34 +/- 9% as single-lined sdB stars at about 25 000-33 000 K. The largest RV-variability fraction of 51 +/- 8% is found in single-lined hot subdwarfs below the canonical EHB. The detected RV-variability fraction of our composite hot subdwarfs with an infrared excess in their spectral energy distributions is 9 +/- 3%, which is lower than that fraction of single-lined hot subdwarfs. Since the average RV uncertainty we measured in the LAMOST spectra is about 7.0 km/s, the lower detected RV-variability fraction for composite hot subdwarfs is expected because the RV amplitudes associated with long-period systems are lower. Conclusions. The results here are generally consistent with the canonical binary evolution channels for forming hot subdwarfs. Most single-lined He-rich hot subdwarfs may form through merger channels, while the stable Roche-lobe overflow channel could play an important role in the formation of composite hot subdwarfs. Single-lined hot subdwarfs with T-eff similar to 35 000-45 000 K located above the EHB may have an evolutionary connection to the sdB stars at about 25 000-33 000 K. The different detected RV-variability fractions for the different subclasses of single-lined hot subdwarfs indicate that their formation channels may differ.
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COMMON ENVELOPE EJECTION ; B-STARS ; GAIA DR2 ; CLOSE BINARY ; SURVIVING COMPANIONS ; SUBLUMINOUS STARS ; KPD 1930+2752 ; SDB-STARS ; IA ; I.
资助项目National Natural Science Foundation of Chian[12288102]; National Natural Science Foundation of Chian[12333008]; National Natural Science Foundation of China[2021YFA1600403]; National Key R&D Program of China[202401BC070007]; National Key R&D Program of China[202201BC070003]; Yunnan Fundamental Research Projects[202302AN360001]; International Centre of Supernovae, Yunnan Key Laboratory[202305AB350003]; Yunnan Revitalization Talent Support Program Science & Technology Champion Project; China Manned Space Project; Chinese Academy of Sciences (CAMS); Guoshoujing Telescope (the Large Sky Area Multi Object Fiber Spectroscopic Telescope LAMOST); National Development and Reform Commission
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001394488200011
出版者EDP SCIENCES S A
资助机构National Natural Science Foundation of Chian[12288102, 12333008] ; National Natural Science Foundation of China[2021YFA1600403] ; National Key R&D Program of China[202401BC070007, 202201BC070003] ; Yunnan Fundamental Research Projects[202302AN360001] ; International Centre of Supernovae, Yunnan Key Laboratory[202305AB350003] ; Yunnan Revitalization Talent Support Program Science & Technology Champion Project ; China Manned Space Project ; Chinese Academy of Sciences (CAMS) ; Guoshoujing Telescope (the Large Sky Area Multi Object Fiber Spectroscopic Telescope LAMOST) ; National Development and Reform Commission
版本出版稿
源URL[http://ir.ynao.ac.cn/handle/114a53/27981]  
专题云南天文台_大样本恒星演化研究组
云南天文台_中国科学院天体结构与演化重点实验室
作者单位1.Physics Department, Xiangtan University, Xiangtan 411105, PR China;
2.International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, PR China;
3.Key Laboratory of Stars and Interstellar Medium, Xiangtan University, Xiangtan 411105, PR China;
4.School of Physics and Astronomy, Sun Yat-sen University, Daxue Road, Zhuhai 519082, PR China
5.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, PR China;
6.University of Chinese Academy of Sciences, Beijing 100049, PR China;
7.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, PR China;
推荐引用方式
GB/T 7714		 He RJ,Meng XC,Lei, Zhenxin,et al. Radial velocity variability fractions of different types of hot subdwarf stars[J]. ASTRONOMY & ASTROPHYSICS,2025,693.
APA 贺锐杰,孟祥存,Lei, Zhenxin,Yan, Huahui,&兰顺义.(2025).Radial velocity variability fractions of different types of hot subdwarf stars.ASTRONOMY & ASTROPHYSICS,693.
MLA 贺锐杰,et al."Radial velocity variability fractions of different types of hot subdwarf stars".ASTRONOMY & ASTROPHYSICS 693(2025).

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