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A post-common-envelope binary with double-peaked Balmer emission lines from TMTS

文献类型：期刊论文

作者Liu, Qichun1; Wang, Xiaofeng1; Lin, Jie1,2,3; Wu CY(吴程远)4,5,6; Li, Chunqian7,8; Filippenko, Alexei V.9; Brink, Thomas G.9; Yang, Yi1,9; Zheng, Weikang9; Liu, Cheng10
刊名Astronomy and Astrophysics
出版日期2025-06-01
卷号698
关键词techniques: radial velocities binaries: spectroscopic stars: evolution white dwarfs stars: winds outflows
ISSN号0004-6361
DOI10.1051/0004-6361/202553732
产权排序第4完成单位
文献子类Article
英文摘要Context. The dynamical method provides an efficient way to discover post-common-envelope binaries (PCEBs) with faint white dwarfs (WDs), thanks to the development of time-domain survey projects. As close binary systems undergo a common-envelope phase, they offer unique opportunities to study the astrophysical processes associated with binary evolution. Aims. We perform a comprehensive analysis of the PCEB system TMTS J15530469+4457458 (J1553), discovered by the Tsinghua University-Ma Huateng Telescopes for Survey, to explore its physical origin and evolutionary fate. Methods. This system is characterized by double-peaked Balmer emission lines, and we applied a cross-correlation function to derive its radial velocity (RV) from a series of phase-resolved Keck spectra. The physical parameters of this binary were obtained by fitting the light curves and RV simultaneously. The locations of the Balmer lines were inferred from Doppler tomography, and a MESA simulation was performed to explore the evolution of this system. Results. Analyses using the cross-correlation function suggest that this system is a single-lined spectroscopic binary and only one star is optically visible. Further analysis through Doppler tomography indicates that J1553 is a detached binary without an accretion disk. Under such a configuration, the simultaneous light-curve and RV fitting reveal that this system contains an unseen WD with mass MA = 0:56 ± 0:09 Mo, and an M4 dwarf with mass MB = 0:37 ±0:02 Mo and radius RB = 0:403+0:014 -0:015 Ro. The extra prominent Balmer emission lines seen in the spectra can trace the motion of the WD; these lines are likely formed near the WD surface as a result of wind accretion. According to the MESA simulation, J1553 could have evolved from a binary consisting of a 2.0-4.0 Mo zero-agemain- sequence star and an M dwarf with an initial orbital period Pi ≈ 201-476 d, and the system has undergone a common-envelope (CE) phase. After about 3:3×106 yr, J1553 should evolve into a cataclysmic variable, with a transient state as a supersoft X-ray source at the beginning. J1553 is an excellent system for studying wind accretion, CE ejection physics, and binary evolution theory. © The Authors 2025.
学科主题天文学
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MINUTE-CADENCE OBSERVATIONS ; MAIN-SEQUENCE BINARIES ; WHITE-DWARF ; LAMOST FIELDS ; DARKENING COEFFICIENTS ; CATACLYSMIC VARIABLES ; STELLAR ; STARS ; MASS ; EVOLUTION
资助项目National Key Research and Development Program of China[12403040]; National Science Foundation of China; Ma Huateng Foundation; Tencent Xplorer Prize[12403038]; National Natural Science Foundation of China[WK2030000089]; Fundamental Research Funds for the Central Universities; Cyrus Chun Ying Tang Foundations[2021YFA1600403]; National Key R&D Program of China; Yunnan Revitalization Talent Support Program-Young Talent project[202302AN360001]; International Centre of Supernovae, Yunnan Key Laboratory; Christopher R. Redlich Fund, Gary and Cynthia Bengier, Clark; Briggs[1242016]; Briggs[24CE-YS-08]; Beijing Natural Science Foundation[24CD012]; Popular Science Project; Beijing Academy of Science and Technology[12173081]; NSFC[ZDBS-LY-7005]; Key research program of frontier sciences, CAS; NASA Explorer Program[NAS 5-26555]; Association of Universities for Research in Astronomy, Inc., under NASA[AST-1440341]; Association of Universities for Research in Astronomy, Inc., under NASA[AST-2034437]; U.S. National Science Foundation (NSF); Weizmann Institute for Science; Oskar Klein Center at Stockholm University; University of Maryland, Deutsches Elektronen-Synchrotron; TANGO Consortium of Taiwan[IN2P3]; Lawrence Livermore National Laboratories; Los Alamos National Laboratories; Lawrence Berkeley National Laboratories
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001498990500012
出版者EDP SCIENCES S A
资助机构National Key Research and Development Program of China[12403040] ; National Science Foundation of China ; Ma Huateng Foundation ; Tencent Xplorer Prize[12403038] ; National Natural Science Foundation of China[WK2030000089] ; Fundamental Research Funds for the Central Universities ; Cyrus Chun Ying Tang Foundations[2021YFA1600403] ; National Key R&D Program of China ; Yunnan Revitalization Talent Support Program-Young Talent project[202302AN360001] ; International Centre of Supernovae, Yunnan Key Laboratory ; Christopher R. Redlich Fund, Gary and Cynthia Bengier, Clark ; Briggs[1242016, 24CE-YS-08] ; Beijing Natural Science Foundation[24CD012] ; Popular Science Project ; Beijing Academy of Science and Technology[12173081] ; NSFC[ZDBS-LY-7005] ; Key research program of frontier sciences, CAS ; NASA Explorer Program[NAS 5-26555] ; Association of Universities for Research in Astronomy, Inc., under NASA[AST-1440341, AST-2034437] ; U.S. National Science Foundation (NSF) ; Weizmann Institute for Science ; Oskar Klein Center at Stockholm University ; University of Maryland, Deutsches Elektronen-Synchrotron ; TANGO Consortium of Taiwan[IN2P3] ; Lawrence Livermore National Laboratories ; Los Alamos National Laboratories ; Lawrence Berkeley National Laboratories
源URL[http://ir.ynao.ac.cn/handle/114a53/28331]  
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, Tsinghua University, Beijing, 100084, China;
2.Cas Key laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei, 230026, China;
3.School of Astronomy and Space Sciences, University of Science and Technology of China, Hefei, 230026, China;
4.Yunnan Observatories, Chinese Academy of Sciences, Kunming, 650216, China;
5.Key Laboratory for Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, 650216, China;
6.International Centre of Supernovae, Yunnan Key Laboratory, Kunming, 650216, China;
7.School of Physics and Astronomy, Beijing Normal University, Beijing, 100875, China;
8.Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing, 102206, China;
9.Department of Astronomy, University of California, Berkeley, CA, 94720-3411, United States;
10.Beijing Planetarium, Beijing Academy of Science and Technology, Beijing, 100044, China;
推荐引用方式
GB/T 7714		 Liu, Qichun,Wang, Xiaofeng,Lin, Jie,et al. A post-common-envelope binary with double-peaked Balmer emission lines from TMTS[J]. Astronomy and Astrophysics,2025,698.
APA Liu, Qichun.,Wang, Xiaofeng.,Lin, Jie.,吴程远.,Li, Chunqian.,...&Yi, Tuan.(2025).A post-common-envelope binary with double-peaked Balmer emission lines from TMTS.Astronomy and Astrophysics,698.
MLA Liu, Qichun,et al."A post-common-envelope binary with double-peaked Balmer emission lines from TMTS".Astronomy and Astrophysics 698(2025).

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