elusive 氦星：亚矮星与沃尔夫-拉耶星之间空隙中的 III. 银河系剥离氦星族的形成
Elusive helium stars in the gap between subdwarfs and Wolf-Rayet stars III. Formation of the Galactic population of stripped helium stars
- Institute of Astronomy, Russian Academy of Sciences（俄罗斯科学院天文研究所）
- Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University（莫斯科国立大学谢尔盖·斯特恩伯格天文研究所）
- Moscow Institute of Physics and Technology（莫斯科物理技术学院）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究通过星族合成方法，基于密近双星演化网格，模拟银河系剥离氦星族形成，估计其数量并分析自转与质量损失影响。
AI中文摘要：
基于预计算的密近双星演化序列网格的星族合成被应用于银河系剥离氦星族形成问题，这些剥离氦星是密近双星中 $5 \lessapprox M/M_\odot \lessapprox 24$ 的主星经过洛希瓣溢流（RLOF）后的残骸。计算中考虑了恒星自转。对于银河系当前恒星形成率 $2\\,M_\odot yr^{-1}$，质量在 1 至 $7\\,M_\odot$ 且有效温度 $T_{eff} \gtrapprox $25000K 的天体数量估计在 14700 到 28500 之间，而质量在 $2\\,M_\odot$ 至 $7\\,M_\odot$ 的天体数量则为 3200 到 5500，具体数值取决于对公共包层形成及其结果的假设。影响估计的其他因素包括采用的恒星形成率、密近双星中主星初始质量分布、质量比分布和轨道周期。观测选择效应可能严重限制可探测天体的数量。剥离氦星伴星的自转角速度约为临界值的 60% 至 80%。使用初始均匀氦星模型作为质量损失后残骸的近似，会导致对前超新星质量的低估。
英文摘要：
Population synthesis based on the grid of pre-computed evolutionary sequences for close binaries is applied to the problem of formation of the Galactic population of stripped helium stars, the remnants of $5 \lessapprox M/M_\odot \lessapprox 24$ primary components of close binaries after RLOF. Stellar rotation is taken into account. For the current star formation rate in the Galaxy $2\,M_\odot yr^{-1}$, the estimate of the number of 1 to $7\,M_\odot$ objects with $T_{eff} \gtrapprox $25000K ranges from 14700 to 28500, while for the number of objects with masses from $2\,M_\odot$ to $7\,M_\odot$ it is 3200 to 5500, depending on the assumptions about formation of common envelopes and their outcomes. Other factors influencing the estimate are adopted star formation rate, distributions of close binaries over initial masses of primary components, mass ratios of components, orbital periods. Observational selection may severely limit the number of detectable objects. Angular velocities of rotation of companions to stripped helium stars are 60 to 80 per cent of the critical one. Using the models of initially homogeneous helium stars as approximations for the remnants after mass loss results in the underestimate of pre-supernovae masses.
