We present the results of wide-band (720-2400 MHz) study of PSR B1821-24A (J1824-2452A, M28A), an energetic millisecond pulsar visible in radio, X-rays and gamma-rays. In radio, the pulsar has a complex average profile which spans >85% of the spin period and exhibits strong evolution with observing frequency. For the first time we measure phase-resolved polarization properties and spectral indices of radio emission throughout almost all of the on-pulse window. We combine this knowledge with the high-energy information to compare M28A to other known gamma-ray millisecond pulsars and to speculate that M28A's radio emission originates in multiple regions within its magnetosphere (i.e. both in the slot or outer gaps near the light cylinder and at lower altitudes above the polar cap). M28A is one of the handful of pulsars which are known to emit Giant Pulses (GPs) -- short, bright radio pulses of unknown nature. We report a drop in the linear polarization of the average profile in both windows of GP generation and also a `W'-shaped absorption feature (resembling a double notch), partly overlapping with one of the GP windows. The GPs themselves have broadband spectra consisting of multiple patches with fractional spectral width ($Δν/ν$) of about 0.07. Although our time resolution was not sufficient to resolve the GP structure on the microsecond scale, we argue that GPs from this pulsar most closely resemble the GPs from the main pulse of the Crab pulsar, which consist of a series of narrowband nanoshots.
Internal superfluid response and torque evolution in the giant glitch of PSR J1718-3718
Qinghai University（青海大学）；Xiamen University（厦门大学）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）；University of Chinese Academy of Sciences（中国科学院大学）
Effects of Alpha-Element Enhancement and the Thermally Pulsing-Asymptotic Giant Branch on Surface Brightness Fluctuation Magnitudes and Broadband Colors
LOFAR observations of the mode-switching pulsar B0943+10
PSR B0943+10是一颗旧的非回收脉冲星，几十年来以其快速和自发的无线电模式切换而闻名。最近，Hermsen等人（2013年）发现了极盖热X射线发射的相关变化，从而证明无线电模式不仅仅是无线电发射区域局部变化的产物，而是某些全球磁层转变的标志。大约在同一时间，由于新一代低频无线电阵列投入使用，可以在电离层透明度窗口的最低边缘进行宽带观测。在这些射频下，PSR B0943+10发射的轮廓形态和单脉冲特性变得非常动态，不仅提供了关于发射本身的细节，而且还提供了关于极隙条件的细节。在这里，我将介绍PSR B0943+10的LOFAR观测的最新结果，并讨论它们对多波长图像的贡献。
Effects of Coronal Mass Ejection on PSR J1022+1001 and Possible Mode Change of PSR J2145-0750 in the InPTA DR2
The Institute of Mathematical Sciences（数学科学研究所）；National Centre for Radio Astrophysics, Tata Institute of Fundamental Research（塔塔基础研究院国家射电天文学中心）；Homi Bhabha National Institute（霍米·巴巴国立研究所）；National Centre for Radio Astrophysics, SP Pune University（SP浦那大学国家射电天文学中心）；Indian Institute of Technology Roorkee（印度理工学院勒克瑙分校（注：通常译为鲁尔基分校））；Kumamoto University（熊本大学）；Indian Institute of Technology Indore（印度理工学院印多尔分校）；IIT Hyderabad（印度理工学院海得拉巴分校）；Indian Institute of Science Education and Research (IISER) Mohali（昌迪加尔印度科学教育与研究学院（莫哈利校区））；University of Mumbai（孟买大学）；Raman Research Institute（拉曼研究所）；North-West University（西北大学）；Indian Institute of Science（印度科学学院）；The Christ (Deemed to be University)（基督大学（被视为大学））；Indian Institute of Technology Delhi（印度理工学院德里分校）；Physical Research Laboratory（物理研究实验室）；IISER Bhopal（博帕尔印度科学教育与研究学院）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（爱因斯坦研究所））；GLA University（GLA大学）
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。
