Discovery of delayed spin-up behavior following two large glitches in the Crab pulsar, and the statistics of such processes
M. Y. Ge, S. N. Zhang, F. J. Lu, T. P. Li, J. P. Yuan, X. P. Zheng, Y. Huang, S. J. Zheng, Y. P. Chen, Z. Chang, Y. L. Tuo, Q. Cheng, C. Güngör, L. M. Song, Y. … 展开作者
M. Y. Ge, S. N. Zhang, F. J. Lu, T. P. Li, J. P. Yuan, X. P. Zheng, Y. Huang, S. J. Zheng, Y. P. Chen, Z. Chang, Y. L. Tuo, Q. Cheng, C. Güngör, L. M. Song, Y. P. Xu, X. L. Cao, Y. Chen, C. Z. Liu, S. Zhang, J. L. Qu, Q. C. Bu, C. Cai, G. Chen, L. Chen, M. Z. Chen, T. X. Chen, Y. B. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. W. Dong, Y. Y. Du, M. X. Fu, G. H. Gao, H. Gao, M. Gao, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, L. F. Hao, J. Huo, S. M. Jia, L. H. Jiang, W. C. Jiang, C. J. Jin, J. Jin, Y. J. Jin, L. D. Kong, B. Li, D. Li, C. K. Li, G. Li, M. S. Li, W. Li, X. Li, X. B. Li, X. F. Li, Y. G. Li, Z. W. Li, Z. X. Li, Z. Y. Liu, X. H. Liang, J. Y. Liao, G. Q. Liu, H. W. Liu, X. J. Liu, Y. N. Liu, B. Lu, X. F. Lu, Q. Luo, T. Luo, X. Ma, B. Meng, Y. Nang, J. Y. Nie, G. Ou, N. Sai, R. C. Shang, X. Y. Song, L. Sun, Y. Tan, L. Tao, C. Wang, G. F. Wang, J. Wang, J. B. Wang, M. Wang, N. Wang, W. S. Wang, Y. D. Wang, Y. S. Wang, X. Y. Wen, Z. G. Wen, B. B. Wu, B. Y. Wu, M. Wu, G. C. Xiao, S. Xiao, S. L. Xiong, Y. H. Xu, W. M. Yan, J. W. Yang, S. Yang, Y. J. Yang, Y. J. Yang, Q. B. Yi, Q. Q. Yin, Y. You, Y. L. Yue, A. M. Zhang, C. M. Zhang, D. P. Zhang, F. Zhang, H. M. Zhang, J. Zhang, T. Zhang, W. C. Zhang, W. Zhang, W. Z. Zhang, Y. Zhang, Y. F. Zhang, Y. J. Zhang, Y. Zhang, Z. Zhang, Z. Zhang, Z. L. Zhang, H. S. Zhao, X. F. Zhao, W. Zheng, D. K. Zhou, J. F. Zhou, X. Zhou, R. L. Zhuang, Y. X. Zhu, Y. Zhu
Glitches correspond to sudden jumps of rotation frequency ($ν$) and its derivative ($\dotν$) of pulsars, the origin of which remains not well understood yet, partly because the jump processes of most glitches are not well time-resolved. There are three large glitches of the Crab pulsar, detected in 1989, 1996 and 2017, which were found to have delayed spin-up processes before the normal recovery processes. Here we report two additional glitches of the Crab pulsar occurred in 2004 and 2011 for which we discovered delayed spin up processes, and present refined parameters of the largest glitch occurred in 2017. The initial rising time of the glitch is determined as $<0.48$ hour. We also carried out a statistical study of these five glitches with observed spin-up processes. The two glitches occurred in 2004 and 2011 have delayed spin-up time scales ($τ_{1}$) of $1.7\pm0.8$\,days and $1.6\pm0.4$\,days, respectively. We find that the $Δν$ vs. $|Δ{\dotν}|$ relation of these five glitches is similar to those with no detected delayed spin-up process, indicating that they are similar to the others in nature except that they have larger amplitudes. For these five glitches, the amplitudes of the delayed spin-up process ($|Δν_{\rm d1}|$) and recovery process ($Δν_{\rm d2}$), their time scales ($τ_{1}$, $τ_{2}$), and permanent changes in spin frequency ($Δν_{\rm p}$) and total frequency step ($Δν_{\rm g}$) have positive correlations. From these correlations, we suggest that the delayed spin-up processes are common for all glitches, but are too short and thus difficult to be detected for most glitches.
IXPE view of the Crab pulsar following the 17 July and 6 August 2025 glitches
INAF Istituto di Astrofisica e Planetologia Spaziali（意大利国家天体物理研究所）；INAF Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze（佛罗伦萨大学物理与天文系）；Istituto Nazionale di Fisica Nucleare, Sezione di Firenze（意大利国家核物理研究院佛罗伦萨分部）；Department of Physics and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学物理系及卡弗里粒子天体物理学与宇宙学研究所）；IRAP, CNRS（法国国家科学研究中心空间研究与行星物理研究所）；INAF Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；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重点实验室）
Braking index of the frequently glitching PSR J0537$-$6910
School of Arts and Sciences, Qingdao Binhai University（青岛滨海学院文理学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Department of Astronomy and Space Sciences, Istanbul University（伊斯坦布尔大学天文学与空间科学系）；Bahçeşehir College（巴切希尔学院）；Faculty of Engineering and Natural Sciences, Sabancı University（萨班哲大学工程与自然科学学院）；Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester（曼彻斯特大学物理与天文学系乔德雷尔银行天体物理学中心）；Departamento de Física, Universidad de Santiago de Chile (USACH)（圣地亚哥智利大学物理系）
Echoes in Different Tempo: Long-Term Monitoring of Crab Echoes with CHIME
David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学戴维·A·邓拉普天文学与天体物理学系）；Canadian Institute for Theoretical Astrophysics（加拿大理论天体物理研究所）；Department of Physics, McGill University（麦吉尔大学物理系）；Trottier Space Institute, McGill University（麦吉尔大学特罗蒂尔太空研究所）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理学与空间研究研究所）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）；Department of Physics and Astronomy, Union College（联合学院物理与天文系）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文学与天体物理学研究所）
Two new outbursts and transient hard X-rays from 1E 1048.1$-$5937
自发现以来，1 E 1048.1 $-$ 5937一直是最活跃的磁星之一，无论是在辐射爆发方面，还是在自旋性质的变化方面。在这里，我们报告了尼尔·盖尔斯斯威夫特天文台X射线望远镜的持续监测活动，其中我们观察到该来源的两次新爆发。第一次爆发发生在2016年7月，第二次爆发发生在2017年12月，分别达到$3.2^{+0.2}_{-0.3}\times 10^{-11}$ erg s $^{-1}$ cm $^{-2}$和$2.2^{+0.2}_{-0.2}\times10^{-11}$ erg s $^{-1}$ cm $^{-2}$的0.5-10 keV吸收通量峰值，$\sim$ 5和$\sim 4$因子高于静态通量。这两个新的爆发都伴随着自旋上升毛刺，幅度分别为$Δν= 4.47(6)\times10^{-7}$ Hz和$Δν= 4.32(5)\times10^{-7}$ Hz。在2016年7月爆发之后，我们观察到，与过去的爆发一样，延迟扭矩波动的一段时间，其达到$1.73\pm0.01$乘以静止速率的峰值自旋下降，并且与自旋上升故障相比，其主导了自旋演化。我们还报告了一个观察的峰值附近的第一个这些爆发与NuSTAR的硬X射线发射被检测到从源。这种发射的特点是吸收的黑体加上一个破幂律，与幂律指数以上的$13.4\pm0.6$千电子伏的$0.5_{-0.2}^{+0.3}$，类似于…
Distinct Modes of Pulsar Glitch Activity Revealed by the Waiting-Time--Amplitude Morphology
State Key Laboratory of Radio Astronomy and Technology, Xinjiang Astronomical Observatory, CAS（中国科学院新疆天文台射电天文与技术重点实验室）；University of Chinese Academy of Sciences（中国科学院大学）；College of Mathematics and Physics, Wenzhou University（温州大学数理学院）；Xinjiang Key Laboratory of Radio Astrophysics（新疆射电天体物理重点实验室）
