2026-09-11 中国科学院（CAS）
Artist’s impression of the pulsar PSR J1921+3745 within the tidal tail of the 8-billion-year-old open cluster NGC 6791. Three telescopes contributed to the study: FAST detected the pulsar, MeerKAT pinpointed its position, and CFHT mapped the surrounding stellar structure. (Image by FU Xiaoting)
＜関連情報＞
- https://english.cas.cn/newsroom/research-news/202609/t20260910_1195122.shtml
- https://www.sciencedirect.com/science/article/abs/pii/S2095927326007504
潮汐剥離によって古代の散開星団から脱出するパルサー
A pulsar escaping an ancient open cluster via tidal stripping
Lei Zhang, Xiaoting Fu, Di Li, Emma Carli, Long Wang, Jiaqi Zhao, Craig O. Heinke, Emanuele Dalessandro, Yang Chen, Angela Bragaglia, Duncan R. Lorimer, Ewan D. Barr, Sarah Buchner, Shi Dai, Zhi-Yu Zhang, Erbil Gügercinoğlu, Alessandro Ridolfi, Jie Zhang, Meng Guo, Mengmeng Ni,…,Qijun Zhi Available online: 7 July 2026
DOI:https://doi.org/10.1016/j.scib.2026.07.006
Most stars are initially formed within star clusters. These stellar systems contribute to the Galactic field population through the escape of individual stars and the gradual dissolution of the clusters over cosmic time. In the Milky Way, the majority of stars in the Galactic disk are thought to have originated in Open Clusters (OCs), whereas halo stars are understood to originate mostly from accreted dwarf galaxies and disrupted globular clusters [1].
Neutron stars (NSs), being the remnants of massive stars, naturally inherit this cluster origin. However, their subsequent retention within or escape from their parent clusters provides a crucial link between small-scale supernova physics and large-scale Galactic tidal interactions. The removal of NSs from OCs is primarily driven by two pathways: tidal interactions with the Galactic gravitational potential and kicks imparted by supernova explosions during their formation. Tidal interactions gradually strip NSs (together with other stars) from clusters as they orbit around the Galaxy, whereas natal kicks from supernovae events can eject NSs effectively [2].
