2025-10-14 中国科学院（CAS）
＜関連情報＞
- https://english.cas.cn/newsroom/research_news/phys/202510/t20251014_1089424.shtml
- https://www.aanda.org/articles/aa/full_html/2025/10/aa55002-25/aa55002-25.html
青色水平分枝星の連星比 The binary fraction of blue horizontal branch stars
Yanjun Guo, Kun Chen, Zhenwei Li, Jie Ju,, Chao Liu, Xiangxiang Xue, Matti Dorsch, Zhanwen Han and XueFei Chen
Astronomy & Astrophysics Published:26 September 2025
DOI:https://doi.org/10.1051/0004-6361/202555002
Abstract
Context. Blue horizontal branch (BHB) stars are old, low-mass, metal-poor stars that serve as important tracers of the Galactic halo structure, kinematics, and evolution. Understanding their binary properties provides key insights into their formation channels and the role of binary interactions in the evolution of horizontal branch stars.
Aims. We investigated the intrinsic binary fraction fbin of BHB stars and its dependences on metallicity, kinematics, and effective temperature.
Methods. We collected 299 BHB stars from LAMOST with multiple radial velocity (RV) measurements and classified the sample into halo-like and disk-like BHBs based on their kinematics and metallicity, and into bluer and redder BHBs based on their effective temperature. We then investigated the observed binary fraction for each group based on the radial velocity variations and applied a set of Monte Carlo simulations, assuming distributions of f(P)∝Pπ and f(q)∝qκ, to correct the observed binary fraction for observational biases and to derive the intrinsic binary fraction.
Results. The observed binary fraction of BHB stars is 18%±2% for cases with n ≥ 2 and 21%±3% for cases with n ≥ 3, where n represents the number of observation times. After correcting for observational biases, the intrinsic binary fraction increases to 31%±3% for n ≥ 2 and 32%±3% for n ≥ 3. A clear contrast is observed between halo-like and disk-like BHB stars, with halo-like BHBs exhibiting a lower intrinsic binary fraction (28%±3% for n ≥ 2 and 29%±3% for n ≥ 3) compared to disk-like BHBs (46%±11% and 51%±11%, respectively), indicating different formation pathways. In particular, halo-like BHB stars are more likely to have formed via a single-star evolution channel, whereas disk-like BHB stars may predominantly result from binary evolution processes. Additionally, we find that bluer BHB stars exhibit a significantly higher binary fraction (42%±6% for n ≥ 2 and 45%±6% for n ≥ 3) than redder BHB stars (24%±5% and 23%±5%, respectively), which suggests a possible link between binarity and the effective temperature, although more samples are required to confirm this. No correlation is found between π (κ) and metallicity or kinematics, nor between π (κ) and the effective temperature of BHB stars.
