Recently, a class of dormant black hole binaries with luminous companions (dBH-LC) has been observed, such as $Gaia$ BH1, BH2, and BH3. Unlike previously discovered X-ray BH binaries, this type of dBH-LC has relatively long orbital periods (typically more than several tens to a few hundred days) and shows very weak X-ray emission. Therefore, studying the formation and evolution of the whole dBH-LC population is also a very interesting problem. Our aim is to study the contribution of massive stars to the dBH-LC population under different evolutionary models (isolated binary evolution (IBE) and hierarchical triple evolution), and different formation channels (such as mass transfer, common envelope evolution). Using the Massive Objects in Binary Stellar Evolution (MOBSE) code, the Triple Stellar Evolution (TSE) code, and the latest initial multiple-star distributions, we model the populations of massive stars. Finally, we calculate the orbital properties, mass distributions, and birthrates of the BH-LC populations formed under these different conditions. In the Milky Way, we calculate that the birthrate of dBH-LC formed through IBE is about 4.35$\times$$10^{-5}$ ${\rm yr}^{-1}$, while the birthrate through triple evolution is about 1.47$\times$$10^{-3}$ ${\rm yr}^{-1}$. This means that the birthrate from triple evolution is one to two orders of magnitude higher than that from IBE. We find that in triple evolution, the main formation channel of dBH-LC is post-merger binaries formed from inner binary mergers triggered by von Zeipel$-$Lidov$-$Kozai oscillations.
Dormant black hole candidates from Gaia DR3 summary diagnostics
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Fakultät für Physik und Astronomie, Universität Heidelberg（海德堡大学物理与天文学院）；Department of Astronomy, California Institute of Technology（加州理工学院天文学系）；Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma（俄克拉荷马大学霍默·L·多格物理与天文学系）；JILA, University of Colorado and National Institute of Standards and Technology（科罗拉多大学与美国国家标准与技术研究院联合JILA实验室）
Discovery of an Extremely Luminous Type II Cepheid in the Andromeda Giant Stellar Stream: Evidence for a Hierarchical Triple with an Inner Binary Merger
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of the Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；South-Western Institute for Astronomy Research, Yunnan University（云南大学西南天文研究所）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿天文与天体物理研究所）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）
Detection of single-degenerate massive binaries with Gaia: The impact of blue supergiants, triples, mass precision, and high-precision parallax requirements
The B[e] Phenomenon in Supergiants. A Result of Mass Transfer in Binaries, Mergers, or What?
University of North Carolina Greensboro（北卡罗来纳大学格林斯伯勒分校）；Fesenkov Astrophysical Institute（费森可夫天体物理研究所）；Al-Farabi Kazakh National University（阿尔法拉比哈萨克国立大学）
The Multiplicity of Massive Stars: A High Angular Resolution Survey with the HST Fine Guidance Sensor
本文介绍了利用哈勃空间望远镜精制导敏感器在大质量恒星中搜寻角分辨双星系统的全天巡天观测结果。224颗恒星的样本主要由银河系的O型和B型恒星和亮蓝变星组成，加上大麦云星云中的一些亮星。FGS TRANS模式观测对角距在0。”01和1。“0并且比$\triangle m = 5$亮。FGS观测分辨了52个双星系统和6个三星系统，并在另外7个目标中探测到部分分辨的双星系统（其中43个是新探测到的）。对于FGS调查，这些数字产生29%的伴随检测频率。我们还收集了文献结果的数量密切的光谱双星和更广泛的天体测量双星之间的样本，我们提出了估计的频率的多个系统和伴侣频率的恒星的子集居住在集群和协会，场星，和失控的明星。这些结果证实了高的多重性分数，特别是在星团和星协中的大质量恒星之间。我们发现，周期分布是近似平坦的对数P的增量。我们确定了一些系统的长期轨道测定的潜在利益，我们注意到的重要性，这些同伴的解释的径向速度和光变曲线的密切的二进制有第三同伴。
MUSCLE W49 : A Multi-Scale Continuum and Line Exploration of the Most Luminous Star Formation Region in the Milky Way. I. Data and The Mass Structure of the Giant Molecular Cloud
