A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
文献类型：期刊论文
| 作者 | Yan, Huahui4,10; Lin, Jiamao4,10; Zheng RZ(郑日中)1,13; Wang, Li4,10; Liu, Genghao4,10; Ren, Liangliang12; Guo, Zhen2,3,6; Xu, Siyi7; Chen, Zhangliang4,10; Chen, Chun4,10 |
| 刊名 | ASTROPHYSICAL JOURNAL LETTERS
 |
| 出版日期 | 2025-09-20 |
| 卷号 | 991期号:1 |
| ISSN号 | 2041-8205 |
| DOI | 10.3847/2041-8213/adfec2 |
| 产权排序 | 第3完成单位 |
| 文献子类 | Article |
| 英文摘要 | White dwarfs (WDs) represent the final evolutionary stage of most stars, typically originating from progenitor stars with masses below approximately 8-10 M circle dot. Formation through single-star evolution generally requires at least 25 Myr, with the youngest WDs often near the Chandrasekhar limit of 1.4 M circle dot. In contrast, WDs formed via binary channels, such as mergers or mass transfer, can develop smaller masses in a shorter timescale and may exhibit unique characteristics, including strong surface magnetic fields and rapid rotation. Accurately determining the ages of these WDs is essential for understanding their formation. A valuable method involves studying WDs in star clusters, where member stars share the same age and chemical composition, allowing for precise constraints on the formation times and metallicities of the WDs' progenitors. Here we report a WD found in the open cluster RSG 5, which is only 35 Myr old. The WD's mass is lower than 1.05 M circle dot, indicating it may not have formed through single-star evolution. The WD possesses an exceptionally strong surface magnetic field (>= 200 MG), a short rotational period (similar to 6.5 minutes), and, most notably, a corotating half-ring of ionized circumstellar debris. This distinctive feature provides evidence for a binary merger origin, a scenario further substantiated by our stellar evolution models. |
| 学科主题 | 天文学 ; 恒星与银河系 |
| URL标识 | 查看原文 |
| 出版地 | No.2 The Distillery, Glassfields, Avon Street, Bristol, ENGLAND |
| WOS关键词 | CONVECTIVE BOUNDARIES ; SPECTRAL EVOLUTION ; VARIABLE-STARS ; STELLAR TRACKS ; GIANT BRANCH ; MASS-LOSS ; MODULES ; ROTATION ; II. ; I. |
| 资助项目 | MOST divided by NSFC divided by Key Programmehttps://doi.org/10.13039/501100010903[12233013]; Natural Science Foundation of China (NSFC)[XDB1160201]; Strategic Priority Research Program of the Chinese Academy of Sciences[12288102]; Strategic Priority Research Program of the Chinese Academy of Sciences[12090043]; Strategic Priority Research Program of the Chinese Academy of Sciences[12173081]; NSFC[2021YFA1600403]; National Key R&D Program of China[202401BC070007]; Yunnan Fundamental Research Projects[202302AN360001]; International Centre of Supernovae, Yunnan Key Laboratory[AIM23-001]; Millennium Science Initiative[2301]; China-Chile Joint Research Fund[E52H540301]; Chinese Academy of Sciences South America Center for Astronomy (CASSACA) Key Research Project[12473034]; National Natural Science Foundation of China; Yunnan Revitalization Talent Support Program-Young Talent Project[202401AT070139]; Yunnan Fundamental Research Project; California Institute of Technology |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:001572900300001 |
| 出版者 | IOP Publishing Ltd |
| 资助机构 | MOST divided by NSFC divided by Key Programmehttps://doi.org/10.13039/501100010903[12233013] ; Natural Science Foundation of China (NSFC)[XDB1160201] ; Strategic Priority Research Program of the Chinese Academy of Sciences[12288102, 12090043, 12173081] ; NSFC[2021YFA1600403] ; National Key R&D Program of China[202401BC070007] ; Yunnan Fundamental Research Projects[202302AN360001] ; International Centre of Supernovae, Yunnan Key Laboratory[AIM23-001] ; Millennium Science Initiative[2301] ; China-Chile Joint Research Fund[E52H540301] ; Chinese Academy of Sciences South America Center for Astronomy (CASSACA) Key Research Project[12473034] ; National Natural Science Foundation of China ; Yunnan Revitalization Talent Support Program-Young Talent Project[202401AT070139] ; Yunnan Fundamental Research Project ; California Institute of Technology |
| 版本 | 出版稿 |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/28583]  |
| 专题 | 云南天文台_大样本恒星演化研究组 |
| 通讯作者 | Ge HW(葛宏伟) |
| 作者单位 | 1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, Yunnan, People’s Republic of China; gehw@ynao.ac.cn; 2.Instituto de Física y Astronomía, Universidad de Valparaíso, Ave. Gran Bretaña, 1111, Casilla 5030, Valparaíso 2520000, Valparaíso, Chile; 3.Millennium Institute of Astrophysics, Nuncio Monseñor Sotero Sanz 100, Of. 104, Providencia, Santiago, Chile; 4.CSST Science Center for the Guangdong-Hongkong-Macau Greater Bay Area, Sun Yat-sen University, DaXue Road, Zhuhai 519082, Guangdong, People’s Republic of China; lichengy5@mail.sysu.edu.cn; 5.Caltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USA; 6.Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK; 7.Gemini Observatory/NSF’s NOIRLab, 670 N. A’ohoku Place, HI 96720, USA; 8.Department of Astronomy, Nanjing University, Xianlin Street, Nanjing 210023, Jiangsu, People’s Republic of China; 9.Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, No.19, Xinjiekouwai Street, Beijing 100875, People’s Republic of China; 10.School of Physics and Astronomy, Sun Yat-sen University, Daxue Road, Zhuhai 519082, Guangdong, People’s Republic of China; |
| 推荐引用方式 GB/T 7714 | Yan, Huahui,Lin, Jiamao,Zheng RZ,et al. A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr[J]. ASTROPHYSICAL JOURNAL LETTERS,2025,991(1). |
| APA | Yan, Huahui.,Lin, Jiamao.,郑日中.,Wang, Li.,Liu, Genghao.,...&Li, Chengyuan.(2025).A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr.ASTROPHYSICAL JOURNAL LETTERS,991(1). |
| MLA | Yan, Huahui,et al."A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr".ASTROPHYSICAL JOURNAL LETTERS 991.1(2025). |
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