A magnetic white dwarf formed through a binary merger within 35 million years
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2025
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| author | Yan, Huahui Lin, Jiamao Zheng, Rizhong Wang, Li Liu, Genghao Ren, Liangliang Guo, Zhen Xu, Siyi Chen, Zhangliang Chen, Chun Ma, Bo Shao, Yong Li, Zhenwei Zhang, Xianfei Fremling, Christoffer Eldridge, Jan J. Ge, Hongwei Li, Chengyuan |
| author_facet | Yan, Huahui Lin, Jiamao Zheng, Rizhong Wang, Li Liu, Genghao Ren, Liangliang Guo, Zhen Xu, Siyi Chen, Zhangliang Chen, Chun Ma, Bo Shao, Yong Li, Zhenwei Zhang, Xianfei Fremling, Christoffer Eldridge, Jan J. Ge, Hongwei Li, Chengyuan |
| contents | White dwarfs (WDs) represent the final evolutionary stage of most stars, typically originating from progenitor stars with masses below approximately 8 $M_{\odot}$ to 10 $M_{\odot}$. Formation through single-star evolution generally requires at least 25 Myr, with the youngest WDs often near the Chandrasekhar limit of 1.4 $M_{\odot}$. 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 $M_{\odot}$, indicating it may not have formed through single-star evolution. The WD possesses an exceptionally strong surface magnetic field ($\ge 200$ MG), a short rotational period ($\sim 6.5$ min), and, most notably, a co-rotating 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. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2509_01069 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A magnetic white dwarf formed through a binary merger within 35 million years Yan, Huahui Lin, Jiamao Zheng, Rizhong Wang, Li Liu, Genghao Ren, Liangliang Guo, Zhen Xu, Siyi Chen, Zhangliang Chen, Chun Ma, Bo Shao, Yong Li, Zhenwei Zhang, Xianfei Fremling, Christoffer Eldridge, Jan J. Ge, Hongwei Li, Chengyuan Solar and Stellar Astrophysics Astrophysics of Galaxies White dwarfs (WDs) represent the final evolutionary stage of most stars, typically originating from progenitor stars with masses below approximately 8 $M_{\odot}$ to 10 $M_{\odot}$. Formation through single-star evolution generally requires at least 25 Myr, with the youngest WDs often near the Chandrasekhar limit of 1.4 $M_{\odot}$. 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 $M_{\odot}$, indicating it may not have formed through single-star evolution. The WD possesses an exceptionally strong surface magnetic field ($\ge 200$ MG), a short rotational period ($\sim 6.5$ min), and, most notably, a co-rotating 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. |
| title | A magnetic white dwarf formed through a binary merger within 35 million years |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2509.01069 |