The study of stripped-envelope core-collapse supernovae (SNe), with evidence for strong interaction of SN ejecta with the circumstellar medium (CSM), provides insights into the pre-supernova progenitor, and a fast-forwarded view of the progenitor mass-loss history. In this context, we present late-time radio observations of SN2004dk, a type Ibc supernova located in the galaxy, NGC 6118, at a distance of $d_L \approx 23$ Mpc. About 15 years after explosion, SN2004dk has shown evidence for H$α$ emission, possibly linked to the SN ejecta interacting with an H-rich CSM. Using data from the VLA Low Band Ionosphere and Transient Experiment (VLITE), we confirm the presence of a late-time radio re-brightening accompanying the observed H$α$ emission. We model the SN2004dk radio light curves within the (spherically symmetric) synchrotron-self-absorption (SSA) model. Within this model, our VLITE observations combined with previously collected VLA data favor an interpretation of SN2004dk as a strongly CSM-interacting radio SN going through a complex environment shaped by a non-steady mass-loss from the SN progenitor.
GRB 080503 late afterglow re-brightening: signature of a magnetar powered merger-nova
GRB 080503是一个由\emph{Swift}探测到的短伽马射线暴（GRB），被归类为致密恒星合并源GRB。在X射线和光学余辉光变曲线中的软扩展发射和同时的后期再增亮引起了关于其物理起源的有趣问题。我们发现，GRB 080503的宽带数据可以很好地解释在双中子星合并模型的框架内，提供的合并残余物是一个快速旋转的大质量中子星具有极高的磁场（即毫秒磁星）。我们表明，后期的光学再增亮是一致的发射从磁星供电的“合并新星”。这为与短伽玛暴相关的并合新星的不断增长的样本又增加了一个案例。软扩展发射和晚期X射线过量发射通过磁星偶极自旋下降光度演化函数很好地联系在一起，表明直接磁耗散是产生这些X射线的机制。X射线辐射最初是从被短伽玛射线暴喷流刺穿的合并喷出物中的一个洞泄漏出来的。在磁星向下旋转并且磁压力下降到冲压压力以下之后，孔随后关闭。然后X射线光子被捕获在合并新星喷出物的后面，直到喷出物在稍后的时间变得光学薄。这解释了光学和X射线光变曲线中基本上同时发生的再增亮。在这个模型中，未来的引力波源可能与一个明亮的X射线对应物以及合并新星相关联，即使短的伽马射线暴喷流远离地球。
Radio Monitoring of the Changing-look AGN Mrk 590 I: VLA Observations Reveal A Bow-shock Driven Radio Brightening Event
University of Copenhagen（哥本哈根大学）；Steward Observatory and Dept. of Astronomy, University of Arizona（亚利桑那大学天文学系斯图尔德天文台）；University of Southampton（南安普顿大学）；Curtin University（科廷大学）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）
First Detection of Radio Polarization During Jet Formation in the Changing-Look AGN 1ES 1927+654
University of Maryland Baltimore County（马里兰大学巴尔的摩县分校）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Center for Space Science and Technology, University of Maryland Baltimore County（马里兰大学巴尔的摩县分校空间科学与技术中心）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA/戈达德太空飞行中心空间科学与探索研究中心）；National Centre for Radio Astrophysics（国家射电天文中心）
Late Engine Activity of GRB 161017A Revealed by Early Optical Observations
GRB 161017 A的长伽马射线暴被费米和斯威夫特探测到，它的余辉被MITSUME 50-cm光学望远镜在爆发后50 s立即观测到。早期的光学观测表明，光学光变曲线表现出一个平台和rebrightening在早期余辉阶段约500和5000秒后，分别触发。通过研究光谱和时间通量变化的行为，发现平台和再增亮不能用简单的标准余辉模型来解释。这些观测特征可以用两个独立的刷新冲击来解释，这表明长期作用的中央引擎。我们评估了后续壳层的物理参数，然后确定两个碰撞壳层与领先壳层的动能比分别约为1和8。此外，两个突出的X射线耀斑约200秒后触发可能是延迟喷射的高能射流负责刷新冲击的签名。中央引擎和X射线耀斑的这种晚期活动在理解喷流形成和光子发射的机制方面起着至关重要的作用。
IGR J12580+0134: A Possible Repeated Partial Tidal Disruption Event Inferred from Late-Time Radio Re-brightenin
Huazhong University of Science and Technology（华中科技大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；University of Science and Technology of China（中国科学技术大学）
Two years of shock interaction tracing three phases of evolution: the explosion of a Type IIn supernova, SN 2019vxm
Indian Institute of Astrophysics（印度天体物理研究所）；Academy of Scientific and Innovative Research (AcSIR)（科学创新研究学院）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）；Amanogawa Galaxy Astronomy Research Center (AGARC), Graduate School of Science and Engineering, Kagoshima University（鹿儿岛大学理工学研究系银河天文研究中心）；Department of Astronomy, Kyoto University（京都大学天文学系）；Hiroshima Astrophysical Science Centre, Hiroshima University（广岛大学广岛天体物理科学中心）；Graduate School of Science and Engineering, Kagoshima University（鹿儿岛大学理工学研究科）
A Delayed Radio Flare Traces Kinetic Energy Injection in the SMBHB Candidate SDSS~J143016.05+230344.4
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Spallation Neutron Source Science Center（散裂中子源科学中心）；Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所粒子天体物理重点实验室）；Department of Physics, Anhui Normal University（安徽师范大学物理系）；CAS Key Laboratory for Researches in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China（中国科学技术大学天文系星系与宇宙学前沿科学中心）；Department of Astronomy, Tsinghua University（清华大学天文系）；Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交通大学李政道研究所）
