We present the flux density measurements of the pulsars observed in the Meterwavelength single-pulse polarimetric emission survey. The average flux densities were estimated in 113 pulsars at two frequencies of 325 and 610 MHz using interferometric imaging. The average profile and single pulse emission in each pulsar were calibrated using the estimated flux density. We have used the flux calibrated average profile to study the variation of the spectral index across the emission beam in 21 pulsars where the core, inner cone and the outer conal components could be clearly identified. The central core component showed a steeper increase in emission at the lower frequency compared with conal emission, with an average difference in spectral index $δα_{core-cone}\sim-0.7$ between the core and the conal components in this frequency range. In contrast the inner conal components had positive difference in their spectral index compared to the outer cones with average difference $δα_{in-out}\sim+0.3$. The variation in the spectral index across the pulse window should provide valuable inputs for constraining the radio emission processes. The single pulse emission showed the presence of emission mode changing in 12 pulsars with 3 cases where the phenomenon is being reported for the first time. In addition we have also detected enhanced emission for short durations or flaring, in parts or across the entire emission window in 14 pulsars. The sudden changes in the emission during mode changing as well as these bursting states are unrelated to the emission mechanism and suggest the presence of rapid and repetitive changes during the plasma generation process.
Meterwavelength Single-pulse Polarimetric Emission Survey. VI. Towards understanding the Phenomenon of Pulsar Polarization in Partially Screened Vacuum Gap model
Detailed Timing, Spectral, and Polarimetric Analysis of Magnetar 1RXS J170849.0-400910
George Washington University（乔治华盛顿大学）；University of Maryland, Baltimore County（马里兰大学巴尔的摩分校）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；Rice University（莱斯大学）；University of Maryland, College Park（马里兰大学帕克分校）；Louisiana State University（路易斯安那州立大学）
Discovery of energy-dependent phase variations in the polarization angle of Cen X-3
State 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国家重点实验室）；University of Chinese Academy of Sciences（中国科学院大学）；Department of Astronomy, University of Geneva（日内瓦大学天文系）
Frequency- and phase-resolved polarimetry of millisecond pulsars and its application to timing
Monash University（莫纳什大学）；OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery（ARC引力波发现卓越中心）；Australia Telescope National Facility, CSIRO（澳大利亚国家望远镜设施，CSIRO）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）；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））；Leibniz Universität Hannover（汉诺威莱布尼茨大学）；Hunan Normal University（湖南师范大学）
Probing the Non-thermal Emission Geometry of AR Sco via Optical Phase-Resolved Polarimetry
AR Sco是一个包含白矮星和红矮星的双星系统。观测到白矮星的自转速度变慢，类似于旋转动力的射电望远镜;因此它被称为“白矮星脉冲星”。我们以前适合传统的无线电脉冲星旋转矢量模型的线性偏振光学数据从这个来源，约束系统的几何形状以及白矮星质量。使用一个更广泛的数据集，我们现在探索应用相同的模型，以二进制相位分辨的光学偏振数据，被认为是非热同步辐射的结果，并推导出磁倾角$α$和观测角$ζ$在不同的轨道相位。我们得到了在轨道周期上$α$的$\sim 10^{\circ}$变化和$ζ$的$\sim 30^{\circ}$变化。这两个参数的变化模式是稳健的，无论所使用的数据的分箱和时期。我们推测，观测者正在检测来自非对称发射区域的辐射，该区域在几个轨道周期内是稳定的结构。最后，这个简单模型的成功意味着粒子的俯仰角很小，脉冲的非热发射起源于相对接近白矮星表面的地方。
XRISM/Resolve observations of Hercules X-1: a pulsating, highly broadened Fe K emission line from the neutron star accretion column
Center for Astrophysics — Harvard & Smithsonian（天体物理中心——哈佛与史密森尼学会）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）；INAF—IASF Palermo（意大利国家天体物理研究所巴勒莫天文物理研究所）；Department of Astronomy and Astrophysics, The University of Chicago（芝加哥大学天体物理学系）；Institut für Astronomie und Astrophysik, Universität Tübingen（蒂宾根大学天文学与天体物理研究所）；Centre for Astrophysics Research, University of Hertfordshire（赫特福德大学天体物理研究中心）；Università degli Studi di Palermo, Dipartimento di Fisica e Chimica（巴勒莫大学物理与化学系）；Institute of Astronomy, Madingley Road, Cambridge（剑桥大学天体物理研究所）；Department of Physics, Graduate School of Science, Kyoto University（京都大学理学研究科物理学系）；Department of Astronomy, University of Michigan（密歇根大学天文学系）
Probing the emission geometry of the X-ray pulsar 2S 1417$-$624 during a weak outburst with NICER, IXPE, and NuSTAR
Institut für Astronomie und Astrophysik, Universität Tübingen（蒂宾根大学天文与天体物理研究所）；Research Center of Astronomy, QingHai University（青海大学天文研究中心）；Department of Physics and Astronomy, QingHai University（青海大学物理与天文系）；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）；University of Chinese Academy of Sciences, Chinese Academy of Sciences（中国科学院大学）
