We study an influence of X-ray photo-ionization from an accreting neutron star in a high mass X-ray binary. Our aim is to unveil a new principle governing X-ray luminosities of X-ray binaries, with a simple analysis of fluid equations simulating line-driven wind flow under influence of X-ray irradiation. In this study, we solve equation of motion of the accretion flow taking into account the line-driven acceleration and X-ray photo-ionization. Under the influence of X-ray irradiation, we find the flow equations take two types of solutions. The first solution is characterized by a slow wind velocity which causes a large accretion rate. The second solution is a fast wind flow which results in a small accretion rate. We find that only the solution with a fast wind and faint X-ray luminosity is a steady solution. On the other hand, slow wind solution with a large X-ray luminosity is not a realizable solution. In bright X-ray binary systems, X-ray luminosity would increase until strong X-ray reduces the line-driven acceleration and causes a stagnation of the wind. This result implies an important consequence that the X-ray luminosity of the wind-fed, X-ray emitting binary will be settled by the wind stagnation limit. At the same time, the fast wind solution with small X-ray luminosity also can be a steady state. Bright X-ray sources, such as Vela X-1, would have limiting luminosities of wind stagnation, while faint systems such a quiescent Super giant Fast X-ray Transients could be on the faint solutions.
The bimodal distribution of donor stars in X-ray binaries
Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences（中国科学院天体结构与演化重点实验室）；Department of Astronomy, Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University（云南大学天文学系，云南省粒子天体物理重点实验室）
本研究通过分析 3,964 个 X 射线双星数据，发现 donor 星参数呈双峰分布，并揭示其背后的“平行轨迹”物理机制，为双星分类提供了数据驱动依据。
The Landscape of Unstable Mass Transfer in Interacting Binaries and Its Imprint on the Population of Luminous Red Novae
University of California, Santa Cruz（加州大学圣克鲁兹分校）；Niels Bohr International Academy, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所、尼尔斯·玻尔国际学院）；Center for Astrophysics, Harvard & Smithsonian（哈佛-史密森天体物理中心）；Institute for Theory and Computation, Harvard & Smithsonian（哈佛-史密森理论计算研究所）
Fragmentation of Dense Rotation-Dominated Structures Fed by Collapsing Gravomagneto-Sheetlets and Origin of Misaligned 100 au-Scale Binaries and Multiple Systems
Measuring the stellar wind parameters in IGR J17544-2619 and Vela X-1 constrains the accretion physics in Supergiant Fast X-ray Transient and classical Supergiant X-ray Binaries
X-ray luminosity function of high-mass X-ray binaries: Studying the signatures of different physical processes using detailed binary evolution calculations
Revealing Optically Hidden Companions to Intermediate-Mass Stripped Stars with Radial Velocities
University of Toronto（多伦多大学）；Dunlap Institute for Astronomy & Astrophysics, University of Toronto（多伦多大学邓普天文学与天体物理研究所）；Institute of Science and Technology Austria (ISTA)（奥地利科学与技术研究院）
Linking high-mass X-ray binaries to binary compact object mergers in Milky Way-like galaxies
Universidad Andres Bello（安德烈斯贝略大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所空间科学与天体物理观测站）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna（拉拉克鲁纳大学）；Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB)（巴塞罗那宇宙科学研究所）；Universität Heidelberg, Zentrum für Astronomie (ZAH), Institut für Theoretische Astrophysik（海德堡大学天文学中心理论天体物理研究所）
Where are the binaries? -- Searching for blue horizontal-branch stars in binary systems in the inner Galactic Halo
Universität Potsdam（波茨坦大学）；University of Warwick（华威大学）；Thüringer Landessternwarte Tautenburg（图林根州陶滕堡天文台）；Astronomical Institute, FAU Erlangen-Nürnberg（埃尔朗根-纽伦堡大学天文研究所）；Astronomical Institute AS CR（捷克科学院天文研究所）
Accretion in Binary Systems with Slow Stellar Winds
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México（墨西哥国立自治大学无线电天文学与天体物理研究所）；SECIHTI–Instituto de Física y Matemáticas, Universidad Michoacana de San Nicolás de Hidalgo（米却肯圣尼古拉斯德伊达尔戈大学物理学与数学研究所）
