A pulsar-like swing in the polarisation position angle of a nearby fast radio burst
Ryan Mckinven, Mohit Bhardwaj, Tarraneh Eftekhari, Charles D. Kilpatrick, Aida Kirichenko, Arpan Pal, Amanda M. Cook, B. M. Gaensler, Utkarsh Giri, Victoria M. … 展开作者
Ryan Mckinven, Mohit Bhardwaj, Tarraneh Eftekhari, Charles D. Kilpatrick, Aida Kirichenko, Arpan Pal, Amanda M. Cook, B. M. Gaensler, Utkarsh Giri, Victoria M. Kaspi, Daniele Michilli, Kenzie Nimmo, Aaron B. Pearlman, Ziggy Pleunis, Ketan R. Sand, Ingrid Stairs, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, Adaeze L. Ibik, Jane F. Kaczmarek, Bikash Kharel, Mattias Lazda, Calvin Leung, Dongzi Li, Robert Main, Kiyoshi W. Masui, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Swarali Shivraj Patil, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Kendrick Smith
Fast radio bursts (FRBs) last for milliseconds and arrive at Earth from cosmological distances. While their origin(s) and emission mechanism(s) are presently unknown, their signals bear similarities with the much less luminous radio emission generated by pulsars within our Galaxy and several lines of evidence point toward neutron star origins. For pulsars, the linear polarisation position angle (PA) often exhibits evolution over the pulse phase that is interpreted within a geometric framework known as the rotating vector model (RVM). Here, we report on a fast radio burst, FRB 20221022A, detected by the Canadian Hydrogen Intensity Mapping Experiment (CHIME) and localized to a nearby host galaxy ($\sim 65\; \rm{Mpc}$), MCG+14-02-011. This one-off FRB displays a $\sim 130$ degree rotation of its PA over its $\sim 2.5\; \rm{ms}$ burst duration, closely resembling the "S"-shaped PA evolution commonly seen from pulsars and some radio magnetars. The PA evolution disfavours emission models involving shocks far from the source and instead suggests magnetospheric origins for this source which places the emission region close to the FRB central engine, echoing similar conclusions drawn from tempo-polarimetric studies of some repeating sources. This FRB's PA evolution is remarkably well-described by the RVM and, although we cannot determine the inclination and magnetic obliquity due to the unknown period/duty cycle of the source, we can dismiss extremely short-period pulsars (e.g., recycled millisecond pulsars) as potential progenitors. RVM-fitting appears to favour a source occupying a unique position in the period/duty cycle phase space that implies tight opening angles for the beamed emission, significantly reducing burst energy requirements of the source.
INTEGRAL/IBIS and optical observations of the Crab nebula/pulsar polarisation
先前的INTEGRAL/IBIS观测表明，蟹状星云的伽马射线辐射是高度偏振的，并且明显地沿着脉冲星的旋转轴排列（Forot et al. 2008）。他们的研究是基于该卫星头四年的运行情况。在这里，我们提出了一个分析的基础上，近十年的运作。这种新的分析允许更好地表征偏振分数和位置角，以及偏振分量的光谱能量分布的测量。然后将这些结果与脉冲星和附近同步加速器结的已知光学偏振进行比较。将来，我们将使用GASP等仪器（Kyne等人，2010年）比较伽马射线偏振与相位分辨光学偏振。
Depolarization Induced by Rapid Polarization Angle Swings: A Common Feature of Pulsars and Fast Radio Bursts?
University of Science and Technology of China（中国科学技术大学）；Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学李政道理论与计算科学中心及物理与天文学院）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）
The MeerKAT Thousand-Pulsar Polarisation Array II: Searches for Ultralight Axion-Like Dark Matter
Stellenbosch University（斯泰伦博斯大学）；Asia Pacific Center for Theoretical Physics (APCTP)（亚太理论物理中心）；Institute of Theoretical Physics, Chinese Academy of Sciences (CAS)（中国科学院理论物理研究所）；The Hong Kong University of Science and Technology（香港科技大学）；Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所）；Center for High Energy Physics, Peking University（北京大学高能物理中心）；University of Manchester（曼彻斯特大学）；Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology（巴塞罗那高等物理研究所（IFAE），巴塞罗那科学技术学院）
A survey for radio pulsars and transients in the 10 pc region around Sgr A*
Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；INAF – Osservatorio Astronomico di Cagliari（意大利国家天体物理研究院卡利亚里天文台）；Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester（曼彻斯特大学物理学与天文学系乔德雷尔银行天体物理学中心）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；State Key Laboratory of Radio Astronomy and Technology（射电天文与技术国家重点实验室）
Magnetospheric birefringence breaks the rotating-vector model and depolarises X-ray pulsars
University College London（伦敦大学学院）；University of Oxford（牛津大学）；University of Turku（图尔库大学）；University of Hertfordshire（赫特福德大学）；University of Padova（帕多瓦大学）
Multi-wavelength emission modelling of PSR~J0437$-$4715
Université de Strasbourg（斯特拉斯堡大学）；Observatoire astronomique de Strasbourg（斯特拉斯堡天文台）；IRAP（天体物理研究所）；LPC2E（地球与环境行星化学与动力学实验室）；Univ Orléans（奥尔良大学）；Observatoire de Paris（巴黎天文台）；Université PSL（巴黎文理研究大学）
Polarised X-ray emission from the accreting millisecond pulsar SAX J1808.4-3658 during an X-ray outburst and a type-I X-ray burst
INAF Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；INAF Istituto di Astrofisica e Planetologia Spaziali（意大利国家天体物理研究所天体物理与空间行星学研究所）；INAF Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究所）
Non-Cosmological FRBs from Young Supernova Remnant Pulsars
我们提出了一个新的河外，但非宇宙学的解释快速射电暴（FRB）的基础上非常年轻的超新星遗迹中的恒星。在几百年的核心崩溃超新星的喷出物被限制在$\sim$ 1 pc，提供了足够高的柱密度的自由电子观测到375-1600 pc cm $^{-3}$的色散措施（DM）。通过在SN 1987 A这样的环境中将一颗类似蟹状星云的脉冲星外推到它的婴儿期，我们假设这样的天体可以偶尔发出超巨星脉冲，这些脉冲的亮度足以在几百兆秒差距内被看到。我们假设，这种超巨星脉冲将优先发生在脉冲星的生命早期，当自由电子密度仍然很高，这就是为什么我们没有看到大量的中等DM FRB（$\lesssim300$ pc cm $^{-3}$）。在这种情况下，源的法拉第旋转给出了比预期的宇宙学贡献大得多的旋转度量（RM）。如果发射是类似脉冲星的，那么偏振矢量可能会在爆发的持续时间内摆动，这在非旋转物体中是不可能的。在这个模型中，散射、大DM和公度RM都来自一个地方，这与宇宙学解释的情况不同。该模型还提供了可测试的预测的流量分布和重复率的FRB，并可以进一步验证的空间重合与光学超新星的过去几十年和交叉相关与附近的星系地图。
On the Difference Between Pulsar Radio Emission Beams from the Two Poles
Guangzhou University（广州大学）；National Astronomical Data Centre, the Great Bay Area, Higher Education Mega Centre（粤港澳大湾区高等教育超算中心国家天文数据中心）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy, University of Chinese Academy of Sciences（中国科学院大学天文学院）
