X-ray emission is an important tracer of stellar magnetic activity. We carried out a systematic correlation analysis for the X-ray luminosity $\log L_{\rm X}$, bolometric luminosity $\log L_{\rm bol}$, and X-ray activity level $\log(L_{\textrm{X}}$/$L_{\textrm{bol}})$ versus the binary parameters including orbital period $P$, Rossby number $R_{\rm O}$, effective temperature $T_{\rm eff}$, metallicity [Fe/H] and the surface gravity $\log g$, and the stellar mass $M$ \& radius $R$, by assembling a large sample of semi-detached (EB-type) binaries with X-ray emission (EBXs). The fact that both $\log L_{\rm X}$ and $\log L_{\rm bol}$ change in accordance with $\log P$ indicates that X-ray emission originates from the convection zone, while $\log L_{\rm X}$ is proportional to the convection zone area. We found that EBXs with main-sequence components exhibit an upward and then a downward trend in both the $\log T_{\rm eff}$-$\log L_{\textrm{X}}$ and $M$-$\log L_{\textrm{X}}$ relations, which is different from the monotonically decreasing trend shown by EBXs containing sub-giant and giant components. The magnetic activity level is negatively correlated with $\log T_{\rm eff}$ and stellar mass. Based on the magnetic dynamo model, the variations in the size and thickness of the surface convection zones can explain the observed relations. EBXs with main-sequence components have similar $R_{\rm O}$-$\log(L_{\textrm{X}}/L_{\textrm{bol}})$ relationship to that of the binaries in the clusters as Praesepe and Hyade. We compared the X-ray radiation properties of EBXs with those of the X-ray-emitting contact binaries and found that EBXs have broader value ranges for $\log L_{\rm X}$ and $\log(L_{\textrm{X}}$/$L_{\textrm{bol}})$.
Chromospheric and Transition Region Responses of activities at the base of Coronal Plumes
Inter University Centre for Astronomy and Astrophysics（大学天文与天体物理中心）；SETI Institute（SETI研究所）；Lockheed Martin Solar and Astrophysics Laboratory（洛马太阳与天体物理实验室）
A Non-Spherical Model for the Solar Coronal Magnetic Field
School of Earth and Space Sciences, Peking University（北京大学地球与空间科学学院）；Center for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven（荷语鲁汶大学数学系等离子体天体物理学中心）；State Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences（中国科学院国家空间科学中心太阳活动与空间天气国家重点实验室）；Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）；University of Newcastle Australia（澳大利亚纽卡斯尔大学）；Mullard Space Science Laboratory, University College London（伦敦大学学院穆拉德空间科学实验室）
What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
FAST Observations of Wave-like Structures in the Radio Dynamic Spectrum of AD Leo
Peking University（北京大学）；National Space Science Center, Chinese Academy of Sciences（中国科学院国家空间科学中心）；ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；University of Groningen（格罗宁根大学）；KU Leuven（荷语鲁汶大学）
High-Resolution Modelling of Coronae and Winds in Solar-type Stars with Varying Rotation Rates I. X-ray Coronae
Nanjing University（南京大学）；Leibniz Institute for Astrophysics Potsdam（波茨坦阿基米德研究所）；SETI Institute（SETI研究所）；University of Potsdam, Institute of Physics and Astronomy（波茨坦大学物理与天文研究所）；Kyoto University（京都大学）；Aalto University（阿尔托大学）；Max-Planck-Institut für Sonnensystemforschung（马克斯·普朗克太阳系统研究所）；Nordita, KTH Royal Institute of Technology & Stockholm University（北欧理论天体物理学中心，瑞典皇家理工学院与斯德哥尔摩大学）
Refinement of global coronal and interplanetary magnetic field extrapolations constrained by remote-sensing and in-situ observations at the solar minimum
针对太阳磁场外推中的 Open Flux Problem，提出三个评估参数结合遥感与就地观测约束日冕和行星际磁场，确定了太阳极小期 PFSS+PFCS 和 CSSS 模型的最优自由参数，发现使用 HMI 综观图可缓解该问题。
Stellar X-ray activity across the Hertzsprung-Russell diagram. I. Catalogs
恒星的磁场活动提供了大量关于磁场发电机和日冕加热过程的信息。本文根据$Chandra$和$Gaia$ DR 2的数据，给出了一个约6000颗恒星的X射线活动目录。我们还将3000多颗恒星分类为年轻恒星、矮星或巨星。利用具有有效恒星参数和分类的恒星，研究了X射线光度（$L_X$）和X射线辐射热光度比（$R_X$）的分布，$L_X$、$R_X$与硬度比的正相关关系，以及X射线的长期变化。该星表可用于研究一些重要的科学主题，包括活动-旋转关系，不同活动指标之间的比较，以及感兴趣对象的活动（例如，A型恒星和巨星）。作为一个例子，我们利用星表研究了活跃度与自转的关系，发现年轻天体、矮星和巨星在$R_X$与Rossby数的关系中落在一个序列上，而巨星不遵循对矮星有效的$R_X$与$P_{\rm rot}^{-2}R^{-4}$的关系。
