发表机构
Universidade de Coimbra; Universidade do Porto; Universidade de Lisboa; Observatoire de Paris, Université PSL, Sorbonne Université; University of Amsterdam（科英布拉大学; 波尔图大学; 里斯本大学; 巴黎天文台，巴黎文理研究大学，索邦大学; 阿姆斯特丹大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
通过动力学建模解释银河系中心S星团双星比例偏低现象，证明潮汐作用导致双星合并或瓦解，支持原位形成假说。
AI 中文摘要
银河系中心的超大质量黑洞人马座A*（Sgr A*）被一个由年轻恒星组成的S星团所环绕。这些恒星主要是B型恒星，但其起源仍不确定。与银河系场中表现出约70%双星比例的巨星不同，S星团中的恒星显示出显著较低的双星比例。理解这一差异对于约束它们的形成至关重要。我们表明，在原位形成情景中，双星赤字自然产生于恒星双星与Sgr A*之间的动力学相互作用。利用K振幅数据，我们推导出S星团恒星的可观测双星比例为f_obs = 0.43 ± 0.09。我们的动力学模型预测，与Sgr A*的相互作用导致18%的双星合并，20%的双星被瓦解，62%的双星幸存，从而产生理论双星比例f_theo = 0.38 ± 0.10。预测的双星比例随与Sgr A*距离的变化也与独立的观测约束一致。这些结果表明，朝向银河系中心双星比例的下降是由更强的潮汐力驱动的，并支持S星团在产生费米气泡的同一事件中原位起源的观点。
英文摘要
The supermassive black hole at the Galactic centre, Sgr A*, is surrounded by an S cluster of young stars. These stars are predominantly B-type stars, but their origin remains uncertain. Unlike massive stars in the Galactic field, which exhibit a binary fraction of about $70\%$, those in the S cluster show a significantly lower fraction. It is key to understand this discrepancy for constraining their formation. We show that the binary deficit arises naturally from dynamical interactions between stellar binaries and Sgr A* in an in situ formation scenario. Using K-amplitude data, we derived an observational binary fraction of $f_{\mathrm{obs}} = 0.43 \pm 0.09$ for the S-cluster stars. Our dynamical modelling predicts that interactions with Sgr A* cause $18\%$ of the binaries to merge, $20\%$ to be disrupted, and $62\%$ to survive, yielding a theoretical binary fraction of $f_{\mathrm{theo}} = 0.38 \pm 0.10$. The predicted binary fraction with distance from Sgr A* is also consistent with independent observational constraints. These results show that the decline in binarity towards the Galactic centre is driven by stronger tidal forces, and they support an in situ origin of the S cluster in the same event that produced the Fermi bubbles.
Comments7 pages; Published in A&A; added Zenodo
Journal refAstronomy & Astrophysics, 712, L15 (2026)
DOI：10.1051/0004-6361/202660648
