X-ray studies of normal late-type galaxies have shown that non-nuclear X-ray emission is typically dominated by X-ray binaries, and provides a useful measure of star formation activity. We have modeled the X-ray evolution of late-type galaxies over the $\sim$ 14 Gyr of cosmic history, with an evolutionary population synthesis code developed by Hurley et al. Our calculations reveal a decrease of the X-ray luminosity-to-mass ratio $L_{\rm X}/M$ with time, in agreement with observations (Fig.~7$a$). We show that this decrease is a natural consequence of stellar and binary evolution and mass accumulating process in galaxies. The X-ray-to-optical luminosity ratio $L_{\rm X}/L_{\rm B}$ is found to be fairly constant (around $\sim 10^{30}$ erg\,s$^{-1}$$L_{\rm B,\odot}^{-1}$, Fig.~7$b$), and insensitive to the star formation history in the galaxies. The nearly constant value of $L_{\rm X}/L_{\rm B}$ is in conflict with the observed increase in $L_{\rm X}/L_{\rm B}$ from $z=0$ to 1.4. The discrepancy may be caused by intense obscured star formation activity that leads to nonlinear relationship between X-ray and B-band emission.
Theoretical expectations for high-mass X-ray binaries, supernova remnants, and their evolutionary paths: An overview talk for LIAC41: the eventful life of stellar multiples
A Path to Constraints on Common Envelope Ejection in Massive Binaries: Full Evolutionary Reconstruction of Three Black Hole X-ray Binaries
International Centre of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research, Yunnan Observatories, Chinese Academy of Sciences (CAS)（中国科学院云南天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Institute of Science and Technology Austria（奥地利科学技术研究所）
Why most neutron star low-mass X-ray binaries accrete transiently: an evolutionary study of transient and persistent phases
Indian Institute of Science Education and Research Bhopal（印度科学教育研究所博帕尔分校）；Tata Institute of Fundamental Research（塔塔基础研究所）；Center for Theoretical Physics（理论物理中心）
On the displacement of X-ray binaries from star clusters in star-burst galaxies
我们用Hurley等人（2000，2002）开发的演化总体合成程序模拟了星暴星系中亮X射线双星从星团中的位移。与Kaaret et al.（2004）一致，我们发现X射线源与其母星系团之间存在显著的空间偏移，并且可以粗略地重建表观X射线亮度与位移的相关性。相关性对簇的基本属性不敏感（例如，初始质量函数的双星）和踢速度赋予新生的紧凑型恒星，除了共同的信封参数。本文给出了当前X射线双星主要参数的分布，这些分布可用于约束未来光学观测中X射线双星形成和演化的模型。
Diagnosing the Properties and Evolutionary Fates of Black Hole and Wolf-Rayet X-ray Binaries as Potential Gravitational Wave Sources for the LIGO-Virgo-KAGRA Network
Anhui Normal University（安徽师范大学）；Université de Genève（日内瓦大学）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Guizhou University（贵州大学）；Zhejiang University of Water Resources and Electric Power（浙江水利水电学院）
The diverse morphology of gravitational wave signals from merging neutron-star white-dwarf binaries
State Key Laboratory of Radio Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台射电天文与技术重点实验室）；CAS Key Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台计算天体物理重点实验室）；School of Astronomy and Space Sciences, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Armagh Observatory and Planetarium（阿马赫天文台和天文馆）；National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences（中国科学院国家天文台/云南天文台）；School of Physical Science and Technology, Lanzhou University（兰州大学物理科学与技术学院）；School of Physics and Technology, Wuhan University（武汉大学物理科学与技术学院）
The metallicity dependence and evolutionary times of merging binary black holes: Combined constraints from individual gravitational-wave detections and the stochastic background
