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A Highly Magnetic Ultramassive White Dwarf with a 23 minute Rotation Period

Jincheng GuoDepartment of Scientific Research, Beijing Planetarium, Xizhimenwai Road, Beijing 100044, People’s Republic of China; [email protected]Xiaofeng WangPhysics Department, Tsinghua University, Beijing 100084, People’s Republic of China; [email protected]Qichun LiuPhysics Department, Tsinghua University, Beijing 100084, People’s Republic of China; [email protected]A. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAThomas G. BrinkDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAJingkun ZhaoKey Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of ChinaWeiKang ZhangDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAYi YangPhysics Department, Tsinghua University, Beijing 100084, People’s Republic of China; [email protected]Jie LinCAS Key laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei, 230026, People’s Republic of ChinaHaowei PengPhysics Department, Tsinghua University, Beijing 100084, People’s Republic of China; [email protected]Hailiang ChenYunnan observatories, Chinese Academy of Sciences (CAS), Kunming, 650216, People’s Republic of ChinaD. O. MirzaqulovUlugh Beg Astronomical Institute, Astronomy Street 33, Tashkent 100052, UzbekistanSh. A. EhgamberdievSamarkand State University, 15, University Boulevard, 140104, Samarkand, UzbekistanBin MaCSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area, Zhuhai 519082, People’s Republic of ChinaJun MoPhysics Department, Tsinghua University, Beijing 100084, People’s Republic of China; [email protected]Cheng LiuDepartment of Scientific Research, Beijing Planetarium, Xizhimenwai Road, Beijing 100044, People’s Republic of China; [email protected]Gaobo XiPhysics Department, Tsinghua University, Beijing 100084, People’s Republic of China; [email protected]Xiaojun JiangUniversity of Chinese Academy of SciencesDanfeng XiangDepartment of Scientific Research, Beijing Planetarium, Xizhimenwai Road, Beijing 100044, People’s Republic of China; [email protected]Jicheng ZhangSchool of Physics and Astronomy, Beijing Normal University, Beijing 100875, People’s Republic of China

2026en

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ABI

Annotatsiya

Abstract We present a physical characterization of Tsinghua University-Ma Huateng Telescope for Survey (TMTS) J00063798+3104160 (J0006), a rapidly rotating, ultramassive white dwarf (WD) identified in high-cadence light curves from the TMTS. A coherent 23 minute periodicity is detected in TMTS, Transiting Exoplanet Survey Satellite, and Zwicky Transient Facility photometry. A time series of low-resolution spectra with the Keck-I 10 m telescope reveals broad, shallow hydrogen absorption features indicative of an extreme magnetic field and shows no evidence for radial-velocity variations. Atmospheric modeling yields a magnetic field strength of ∼250 MG, while Gaia astrometry and photometry imply a mass of 1.06 ± 0.01 M ⊙ . A significant infrared excess is detected in the Wide-field Infrared Survey Explorer W1 band and is well fitted by a 550 K blackbody, likely arising from residual material of a merger. We interpret the 23 minute photometric modulation as the rotation period of an isolated, massive WD formed likely through the merger of a double WD binary. With one of the shortest rotation periods known among candidate merger remnants and with constraints from a deep Einstein Probe X-ray nondetection, J0006 provides a rare and important observational window into the poorly explored intermediate stages of postmerger evolution.

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DOI: 10.3847/1538-4357/ae3a7a

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