We present a kinematic and dynamical analysis of six Galactic open clusters NGC~2204, NGC~2660, NGC~2262, Czernik~32, Pismis~18, and NGC~2437, using \textit{Gaia}~DR3. We used Bayesian and Gaussian Mixture Model (GMM) methods to identify cluster members, but chose GMM because it's more appropriate for low-mass stars. Estimated distances range from 1.76 to 4.20~kpc and ages from 0.199 to 1.95~Gyr, confirming their intermediate-age nature. King model fits indicate compact morphologies, with core radii of 1--10~arcmin and cluster radii of 5--24~arcmin. We identify 13 BSS and 3 YSS members, whose central concentrations suggest origins via mass transfer or stellar collisions. The mass function slopes (0.96--1.19) are flatter than the Salpeter value, which indicates that these clusters have undergone dynamical mass segregation. Orbit integration within a Galactic potential indicates nearly circular orbits (eccentricities 0.02--0.10), vertical excursions within $\pm$132~pc, and guiding radii near the solar circle, suggesting disk confinement. These clusters likely formed in the thin disk and are shaped by Galactic tidal perturbations, facilitating the rapid loss of low-mass members. Additionally, twelve variable stars were found across four clusters using \textit{TESS} light curves, including $γ$~Doradus and SPB pulsators, eclipsing binaries, and a yellow straggler candidate. Periods were derived via Lomb-Scargle analysis. Two eclipsing binaries (TIC~94229743 and TIC~318170024) were modeled using PHOEBE, yielding mass ratios of 1.37 and 2.16, respectively. Our findings demonstrate that integrating orbital dynamics and variable star studies presents valuable insights into the evolutionary pathways of open clusters.
Unveiling Vela -- Variability of Interstellar Lines in the Direction of the Vela Supernova Remnant III. Na D and Ca II K
2017年至2019年，南部非洲大型望远镜在船帆座超新星遗迹的方向上获得了15颗恒星的高分辨率光谱。本文讨论了星际Ca i H、K和Na i D线。特别是，线配置文件进行比较，在1993-1996年获得的Cha和Sembach的光谱分辨率的配置文件。其中10条视线显示了该视线中一个或多个组件的变化。变化包括在两次观测期间之间的二十年间径向速度的微小变化（1-2公里/秒）和（或）等效宽度的增加/减少。Ca-K线的变化比Na-D线的变化更明显。这些变化归因于超新星喷出物和周围星际介质之间相互作用所扰动的气体。典型的时间尺度可以是20-50年。如前所述，遗迹表面线剖面的小尺度变化表明，相互作用的线性尺度是目前遗迹40 pc大小的一小部分。
The THESAN-ZOOM project: Burst, quench, repeat -- unveiling the evolution of high-redshift galaxies along the star-forming main sequence
Kavli Institute for Cosmology, University of Cambridge（卡弗里宇宙学研究所，剑桥大学）；Cavendish Laboratory, University of Cambridge（卡文迪许实验室，剑桥大学）；Department of Physics, The University of Texas at Dallas（德克萨斯大学达拉斯分校物理系）；Department of Physics and Astronomy, York University（约克大学物理与天文系）；Leibniz-Institut für Astrophysik Potsdam（波茨坦阿斯特拉诺伊克莱布尼茨研究所）；Department of Physics and Astronomy, University of Pennsylvania（宾夕法尼亚大学物理与天文系）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学 Kavli 宇宙物理学与数学起源联合研究中心（WPI），UTIAS）；Institute for Fundamental Physics of the Universe（宇宙基本物理研究所）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天文学研究所）
25 Years of Mrk 421 with XMM-Newton: Unveiling Structured Jets and Energy-Dependent Escape
School of Astronomy and Space Science, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）；Janusz Gil Institute of Astronomy, University of Zielona Góra（绿山城大学扬努什·吉尔天文学研究所）；Doctoral School of Exact and Technical Sciences, University of Zielona Góra（绿山城大学精确与技术科学博士学院）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）
基于 XMM-Newton 25 年观测，对 Mrk 421 进行 X 射线光谱与变率分析，发现硬变率更强、通量分布类对数正态，且光谱需用断裂幂律或对数抛物线描述，支持结构化喷流或能量依赖逃逸模型。
Unveiling the dynamics of the ultra-fast outflow in IRAS 13224-3809 with X-ray spectroscopy
Università di Roma Tor Vergata（罗马托尔维加塔大学）；INFN - Rome Tor Vergata（罗马托尔维加塔国家核物理研究所）；INAF - Osservatorio Astronomico di Roma（罗马天文台意大利国家天体物理研究所）；INAF - Istituto di Astrofisica e Planetologia Spaziali（空间天体物理学和行星科学研究所意大利国家天体物理研究所）；Space Science Data Center, Agenzia Spaziale Italiana（意大利航天局空间数据中心）
Unveiling Massive Main-Sequence Stars in Sextans A through Panchromatic Photometry
The Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；California Institute of Technology（加州理工学院）；University of California, Berkeley（加州大学伯克利分校）；NSF National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）；University of Washington（华盛顿大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；Flatiron Institute（平托研究所）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
