A few fast radio bursts' (FRBs) light-curves have exhibited large intrinsic modulations of their flux on extremely short ($t_{\rm r}\sim 10μ$s) time scales, compared to pulse durations ($t_{\rm FRB}\sim1$ms). Light-curve variability timescales, the small ratio of rise time of the flux to pulse duration, and the spectro-temporal correlations in the data constrain the compactness of the source and the mechanism responsible for the powerful radio emission. The constraints are strongest when radiation is produced far ($\gtrsim 10^{10}$cm) from the compact object. We describe different physical set-ups that can account for the observed $t_{\rm r}/t_{\rm FRB}\ll 1$ despite having large emission radii. The result is either a significant reduction in the radio production efficiency or distinct light-curves features that could be searched for in observed data. For the same class of models, we also show that due to high-latitude emission, if a flux $f_1(ν_1)$ is observed at $t_1$ then at a lower frequency $ν_2<ν_1$ the flux should be at least $(ν_2/ν_1)^2f_1$ at a slightly later time ($t_2=t_1ν_1/ν_2$) independent of the duration and spectrum of the emission in the comoving frame. These features can be tested, once light-curve modulations due to scintillation are accounted for. We provide the timescales and coherence bandwidths of the latter for a range of possibilities regarding the physical screens and the scintillation regime. Finally, if future highly resolved FRB light-curves are shown to have intrinsic variability extending down to $\sim μ$s timescales, this will provide strong evidence in favor of magnetospheric models.
A Search for Rotation Measure Flare Candidates in Repeating Fast Radio Bursts
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；State Key Laboratory of Radio Astronomy and Technology, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台射电天文与技术重点实验室）
A broadband study of FRB20240114A with the Effelsberg 100-m radio telescope
Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Argelander Institute for Astronomy（阿根兰德天文学研究所）；Julius-Maximilians-Universität Würzburg（维尔茨堡朱利叶斯-马克西米利安大学）；University of Potsdam（波茨坦大学）；Joint Institute for VLBI ERIC（甚长基线干涉测量联合研究所）
Constraining the origin of the long term periodicity of FRB 20180916B with Polarization Position Angle
Max-Planck-Institute for Radio Astronomy（马克斯·普朗克射电天文研究所）；Princeton University（普林斯顿大学）；McGill University（麦吉尔大学）；Trottier Space Institute, McGill University（麦吉尔大学特罗蒂尔空间研究所）
本研究利用uGMRT观测的FRB 20180916B偏振位置角数据，约束其长周期起源，排除了各类进动模型，发现其与X射线双星Her X 1的偏振变化特征相似。
Statistical and Temporal Analysis of Multi-component Burst-clusters from the Repeating FRB 20190520B
Institute of Astrophysics, Central China Normal University（华中师范大学天体物理研究所）；Education Research and Application Center, National Astronomical Data Center（国家天文台教育研究与应用中心）；Key Laboratory of Quark and Lepton Physics (Central China Normal University), Ministry of Education（教育部夸克与轻子物理重点实验室（华中师范大学））；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Department of Astronomy, Tsinghua University（清华大学天文系）；Research Center for Astronomical Computing, Zhejiang Laboratory（浙江实验室天文计算研究中心）；Institute for Astronomy, School of Physics, Zhejiang University（浙江大学物理学院天体物理研究所）
Continued radio observations of the persistent radio source associated with FRB20190520B provides insights into its origin
Indian Institute of Astrophysics（印度天体物理研究所）；Tata Institute of Fundamental Research（塔塔基础研究所）；Carnegie Mellon University（卡内基梅隆大学）；National Centre for Radio Astrophysics（国家射电天体物理中心）
A steadily declining dispersion measure for the repeating fast radio burst FRB 20220529A: Evidence for an FRB engine embedded in an expanding supernova remnant
McGill University（麦吉尔大学）；University of Toronto（多伦多大学）；Northwestern University（西北大学）；Massachusetts Institute of Technology（麻省理工学院）
Searching for links between energetic millisecond pulsars and repeating fast radio bursts
Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内科克天文学研究所）；ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所 ASTRON）；Department of Physics, McGill University（麦吉尔大学物理系）；Trottier Space Institute, McGill University（麦吉尔大学特罗蒂尔太空研究所）；Joint institute for VLBI ERIC（甚长基线干涉测量联合研究所 ERIC）；CSIRO Space and Astronomy, Australia Telescope National Facility（澳大利亚联邦科学与工业研究组织空间与天文部，澳大利亚望远镜国家设施）
Search for persistent radio emission towards selected localised Fast Radio Burst positions using the MeerKAT Telescope
North-West University（西北大学）；National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）；University of South Africa（南非大学）；University of Nigeria（尼日利亚大学）；SKA Observatory（平方公里阵列射电望远镜天文台）
A MeerKAT search for persistent radio sources towards twenty-five localised Fast Radio Bursts
North-West University（西北大学）；University of South Africa（南非大学）；University of Nigeria（尼日利亚大学）；National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）；South African Radio Astronomy Observatory（南非射电天文台）；Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester（曼彻斯特大学物理与天文学系乔德雷克天体物理学中心）
On the polarization position angle jumps in FRB 20240114A
Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内克天体物理研究所）；ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所 ASTRON）；Trottier Space Institute, McGill University（麦吉尔大学特罗蒂尔太空研究所）；Department of Physics, McGill University（麦吉尔大学物理系）；LPC2E, OSUC, Univ Orléans, CNRS, CNES（奥尔良大学/法国国家科学研究中心/法国国家空间研究中心 LPC2E 实验室）
A fast radio burst cyclone in technicolour: evidence of plasma lensing
Swinburne University of Technology（斯威本科技大学）；ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav)（引力波发现卓越研究中心（OzGrav））；CSIRO（澳大利亚联邦科学与工业研究组织）；Australia Telescope National Facility, CSIRO, Space and Astronomy（CSIRO空间与天文部澳大利亚望远镜国家设施）；Weizmann Institute of Science（魏茨曼科学研究所）；Stanford University（斯坦福大学）；Kavli Institute for Particle Astrophysics & Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）
PSR B0950+08是一颗明亮的非回收脉冲星，据报道其单脉冲通量变化很大。基于两个相距甚远的频率，55 MHz（NenuFAR）和1.4 GHz（Westerbork综合射电望远镜）的观测，我们回顾了这些单脉冲的性质。我们的结论是，它们更类似于普通的无线电发射脉冲，而不是一种特殊的短而明亮的巨脉冲，只从少数几颗恒星中观察到。我们认为，沿视线的星际介质的属性的时间变化，这附近的脉冲星，即衍射闪烁的去相关带宽的波动大小作出了重要的贡献，观察到的单脉冲注量的变化。我们进一步提出了有趣的结构，在低频单脉冲光谱，类似于“悲伤长号”看到的快速射电暴（FRB），虽然PSR B0950+08的向上频率漂移也经常存在。我们用半径到频率映射来解释这些光谱特征，类似于Wang等人开发的模型。（2019）FRB。最后，我们推测，微秒尺度的一般脉冲星人口的通量变化仍然知之甚少，它的进一步研究可能会带来重要的线索FRB的性质。
A Missing Tool for Calculating Auto/Cross-correlation Function under Nonuniform Sampling Observations
School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education（教育部现代天文与天体物理重点实验室（南京大学））；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Institute of Space Weather, School of Atmospheric Physics, Nanjing University of Information Science and Technology（南京信息工程大学大气物理学院太空天气研究所）；Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University（广西大学物理科学与技术学院相对论天体物理广西壮族自治区重点实验室）；State Key Laboratory of Radio Astronomy and Technology, NAOC, Chinese Academy of Sciences（中国科学院国家天文台射电天文与技术国家重点实验室）
OVRO 40 m Blazar Monitoring Program: Location of the gamma-ray emission region in blazars by the study of correlated variability at radio and gamma-rays
Detection of giant pulses from the transitional millisecond pulsar J1227$-$4853
National Centre for Radio Astrophysics, Tata Institute of Fundamental Research（国家射电天文中心，塔塔基础研究所）；Space Science Division, U.S. Naval Research Laboratory（空间科学处，美国海军研究实验室）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester（曼彻斯特大学物理与天文学系乔德雷尔银行天体物理学中心）
