YNAO OpenIR  > 大样本恒星演化研究组
Hot Subdwarf Stars Observed in Gaia DR2 and LAMOST DR5
Luo, Yangping1; Nemeth, Peter2,3; Deng, Licai1,4; Han ZW(韩占文)5
发表期刊ASTROPHYSICAL JOURNAL
2019-08-10
卷号881期号:1页码:16
DOI10.3847/1538-4357/ab298d
产权排序第5完成单位
收录类别SCI
关键词stars: kinematics and dynamics subdwarfs surveys
摘要

Combing Gaia DR2 with LAMOST DR5, we spectroscopically identified 924 hot subdwarf stars, among which 32 stars exhibit strong double-lined composite spectra. We measured the effective temperature T-eff, surface gravity logg, helium abundance y = nHe/nH, and radial velocities of 892 non-composite spectra hot subdwarf stars by fitting LAMOST observations with Tlusty/Synspec non-LTE synthetic spectra. We outlined four different groups in the T-eff-logg diagram with our helium abundance classification scheme and two nearly parallel sequences in the T-eff-log(y) diagram. 3D Galactic space motions and orbits of 747 hot subdwarf stars with (G(BP) - G(RP))(0) < -0.36 mag were computed using LAMOST radial velocities and Gaia parallaxes and proper motions. Based on the U - V velocity diagram, J(z)-eccentricity diagram, and Galactic orbits, we derived Galactic population classifications and the fractional distributions of the four hot subdwarf helium groups in the halo, thin disk and thick disk. Comparisons with the predictions of binary population synthesis calculations (Han 2008) suggest that He-rich hot subdwarf stars with log(y) >= 0 are from the double helium white dwarfs merger, He-deficient hot subdwarf stars with -2.2 <= log(y) < -1 from the common envelope ejection, and He-deficient hot subdwarf stars with log(y) < -2.2 from the stable Roche lobe overflow channels. The relative number of He-rich hot subdwarf stars with -1 <= log(y)<0 and log(y) >= 0 in the halo is more than twice the prediction of Zhang et al.(2017), even more than six times in the thin disk, which implies that the mergers of helium white dwarfs with low mass main sequence stars may not be the main formation channel of He-rich hot subdwarf stars with - 1 <= log(y) < 0, specially in younger environments.

资助项目National Natural Science Foundation of China[U1731111] ; National Natural Science Foundation of China[11521303] ; National Natural Science Foundation of China[11733008] ; Grant Agency of the Czech Republic[GACR 18-20083S] ; foundation of Yunnan province[2017HC018] ; National Development and Reform Commission
项目资助者National Natural Science Foundation of China[U1731111, 11521303, 11733008] ; Grant Agency of the Czech Republic[GACR 18-20083S] ; foundation of Yunnan province[2017HC018] ; National Development and Reform Commission
语种英语
学科领域天文学 ; 恒星与银河系 ; 恒星天文学
学科门类理学 ; 理学::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
ISSN0004-637X
URL查看原文
WOS记录号WOS:000479099500007
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]BLANKETED MODEL ATMOSPHERES ; IA PROGENITOR SURVEY ; BLUE HOOK STARS ; WHITE-DWARFS ; B-STARS ; RICH SUBDWARFS ; 3D KINEMATICS ; BINARIES ; SELECTION ; ORIGIN
引用统计
被引频次:24[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/20964
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
通讯作者Luo, Yangping
作者单位1.Department of Astronomy, China West Normal University, Nanchong, 637002, People's Republic of China
2.Astronomical Institute of the Czech Academy of Sciences, CZ-25165, Ondr̆ejov, Czech Republic
3.Astroserver.org, 8533 Malomsok, Hungary
4.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China
5.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, People's Republic of China
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Luo, Yangping,Nemeth, Peter,Deng, Licai,et al. Hot Subdwarf Stars Observed in Gaia DR2 and LAMOST DR5[J]. ASTROPHYSICAL JOURNAL,2019,881(1):16.
APA Luo, Yangping,Nemeth, Peter,Deng, Licai,&Han ZW.(2019).Hot Subdwarf Stars Observed in Gaia DR2 and LAMOST DR5.ASTROPHYSICAL JOURNAL,881(1),16.
MLA Luo, Yangping,et al."Hot Subdwarf Stars Observed in Gaia DR2 and LAMOST DR5".ASTROPHYSICAL JOURNAL 881.1(2019):16.
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