We present a detailed spectral and timing analysis of X-ray observations of the brightest eclipsing systems Alpha Coronae Borealis taken by XMM-Newton. We got from the thermal plasma model metal the abundances of some elements (O, Mg, Si, and Fe) and an emission line at 1.3 Kev from the simple Gaussian line profile. From the light curves, there is a strong active region at the lower left in the maps, near the limb of the G component, and increasing in some parts which means a band diagonally running across the G star disk from lower left to upper right, close to the projected center.
Probing the potential high-energy messengers of the anticipated T Coronae Borealis outburst
INAF - Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；Institute for Applied Problems in Mechanics and Mathematics, National Academy of Sciences of Ukraine（乌克兰国家科学院应用力学与数学问题研究所）；Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University（密歇根州立大学物理与天文学系数据密集型时域天文中心）；Dipartimento di Fisica e Chimica E. Segrè, Università degli Studi di Palermo（巴勒莫大学E. Segre物理化学系）
When will T Coronae Borealis next erupt as a nova? Constraints from recurrence, orbital phase, and accretion-state evolution
Liupanshui Normal University（六盘水师范学院）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学汤正道研究院）；Yunnan Observatories, Chinese Academy of Sciences (CAS)（中国科学院云南天文台）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Qiannan Normal University for Nationalities（黔南民族师范学院）；Guizhou University（贵州大学）；Xi’an Jiaotong University（西安交通大学）
Radio component of the multi-messenger emission from the anticipated T Coronae Borealis outburst
INAF - Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；Institute for Applied Problems in Mechanics and Mathematics, National Academy of Sciences of Ukraine（乌克兰国家科学院应用力学与数学问题研究所）；Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University（密歇根州立大学物理与天文学系数据密集与时域天文中心）；Dipartimento di Fisica e Chimica E. Segrè, Università degli Studi di Palermo（巴勒莫大学E. Segrè物理化学系）
Multi-wavelength study of the pre-eruption dip in the recurrent nova T Coronae Borealis preceding imminent nova eruption
Liupanshui Normal University（六盘水师范学院）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）；Qiannan Normal University for Nationalities（黔南民族师范学院）
Dissecting a disk-instability outburst in a symbiotic star: $NuSTAR$, and $Swift$ observations of T Coronae Borealis during the rise to the "super-active" state
Predicting the X-ray signatures of the imminent T Coronae Borealis outburst through 3D hydrodynamic modeling
INAF – Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University（密歇根州立大学物理与天文学系数据密集型与时域天文中心）；Lockheed Martin Solar and Astrophysics Laboratory（洛基德马丁太阳与天体物理学实验室）；Dip. di Fisica e Chimica E. Segrè, Università degli Studi di Palermo（巴勒莫大学E. Segrè物理化学系）；Institute for Applied Problems in Mechanics and Mathematics（力学与数学应用问题研究所）
California Institute of Technology（加州理工学院）；Clemson University（克莱姆森大学）；Flatiron Institute（平顿研究所）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；Montana State University（蒙大拿州立大学）；Università di Bologna（博洛尼亚大学）；INAF–OAA, Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所-阿切特里天文台）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Columbia University（哥伦比亚大学）
Fast X-ray Variability from the Coronae of Supermassive Black Holes
California Institute of Technology（加州理工学院）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Columbia University（哥伦比亚大学）；Clemson University（克莱姆森大学）
