A pulsar-helium star compact binary system formed by common envelope evolution

• 成果类型: Article
• 署名作者: Yang, Z. L.; Han, J. L.; Zhou, D. J.; Jing, W. C.; Chen, W. C.; Wang, T.; Li, X. D.; Wang, S.; Wang, B.; Ge, H. W.; Guo, Y. L.; Li, L. H.; Shao, Y.; Liu, J. F.; Su, W. Q.; Hou, L. G.; Huang, W. J.; Jiang, J. C.; Jiang, P.; Sun, J. H.; Wang, B. J.; Wang, C.; Wang, H. G.; Wang, J. B.; Wang, N.; Wang, P. F.; Wang, S. Q.; Xu, H.; Xu, J.; Xu, R. X.; Yan, W. M.; Yan, Y.; You, X. P.; Yu, D. J.; Yuan, Z. S.; Zhang, C. F.
• 署名单位: Chinese Academy of Sciences; National Astronomical Observatory, CAS; Chinese Academy of Sciences; University of Chinese Academy of Sciences, CAS; Qingdao University of Technology; Nanjing University; Nanjing University; Chinese Academy of Sciences; Yunnan Astronomical Observatory, NAOC, CAS; Sun Yat Sen University; Guangzhou University; Chinese Academy of Sciences; Xinjiang Astronomy Observatory, CAS; Peking University; Southwest University - China
• 刊物名称: SCIENCE
• ISSN/ISSBN: 0036-8676
• DOI: 10.1126/science.ado0769
• 发表日期: 2025-05-22
• 页码: 859-863
• 关键词: white-dwarf companions; millisecond pulsars; orbital parameters; neutron; supernovae; progenitors; accretion; cores

摘要

A stellar common envelope occurs in a binary system when the atmosphere of an evolving star expands to encompass an orbiting companion object. Such systems are predicted to evolve rapidly, ejecting the stellar envelope and leaving the companion in a tighter orbit around a stripped star. We used radio timing to identify a pulsar, PSR J1928+1815, with a spin period of 10.55 ms in a compact binary system with an orbital period of 3.60 hours. The companion star has 1.0 to 1.6 solar masses, eclipses the pulsar for about 17% of the orbit, and is undetected at other wavelengths, so it is most likely a stripped helium star. We interpret this system as having recently undergone a common envelope phase, producing a compact binary.