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

作者：Qichun Liu, Xiaofeng Wang, Jie Lin, Chengyuan Wu, Chunqian Li, A. V. Filippenko, Thomas G. Brink, Yi Yang, WeiKang Zheng, Cheng Liu, Cuiying Song, Mikhail Kovalev, Hongwei Ge, Fenghui Zhang, Xiaobin Zhang, Qiqi Xia, Haowei Peng, Gaobo Xi, Jun Mo, Shengyu Yan, Jianrong Shi, Jiangdan Li, Tuan Yi · 发表于：Astronomy and Astrophysics · 年份：2025 · DOI：10.1051/0004-6361/202553732 · 被引用次数：2 · 研究领域：Stellar, planetary, and galactic studies、Astronomy and Astrophysical Research、Astrophysics and Star Formation Studies

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 M A = 0.56±0.09 M ⊙ , and an M4 dwarf with mass M B = 0.37±0.02 M ⊙ a...