发表机构
Macquarie University; Australia Telescope National Facility, CSIRO; OzGrav: The ARC Center of Excellence for Gravitational Wave Discovery; Xinjiang Astronomical Observatory, Chinese Academy of Sciences; School of Physics and Astronomy, Monash University（麦考瑞大学; 澳大利亚望远镜国家设施，CSIRO; OzGrav：ARC引力波发现卓越中心; 中国科学院新疆天文台; 蒙纳士大学物理与天文学学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用七年观测数据发现毫秒脉冲星PSR J0437-4715存在两个连续的轮廓变化事件，证实其磁层起源，为发射模型提供新约束。
AI 中文摘要
最近且最亮的毫秒脉冲星（MSP）PSR J0437-4715是精密计时实验（包括帕克斯脉冲星计时阵列（PPTA）项目）中的高优先级脉冲星，在该项目中它既用于脉冲星计时，也用于偏振校准。利用在CSIRO的帕克斯射电望远镜Murriyang上使用超宽带低频接收机获得的约七年的观测数据，我们研究了PSR J0437-4715的长期光谱偏振变异性。我们报告发现了两个连续的离散轮廓变化事件，它们表现出相同的相位局域形态变化，这是在任何MSP中首次报道的这种行为。这两个事件都影响脉冲轮廓的三个相位局域区域，这些区域表现出耦合且反相关的时间演化。我们还识别并纠正了由接收机偏振特性长期漂移引起的偏振校准误差所导致的系统性轮廓变异性。轮廓变化在总强度中表现出频率依赖的演化，同时伴有线性偏振、位置角和分数线性偏振的变化。这些结果证实了这些事件的磁层起源，而非星际介质引起的传播效应，并为MSP发射模型提供了潜在的新约束。
英文摘要
The closest and brightest millisecond pulsar (MSP), PSR J0437-4715, is a high-priority pulsar for precision timing experiments, including the Parkes Pulsar Timing Array (PPTA) project, where it is used for both pulsar timing and for polarization calibration. Using approximately seven years of observations obtained with the Ultra-Wideband Low-Frequency receiver on Murriyang, CSIRO's Parkes radio telescope, we investigate the long-term spectro-polarimetric variability of PSR J0437-4715. We report the discovery of two consecutive discrete profile change events exhibiting the same phase-localised morphological variations, the first such behaviour reported in any MSP. Both events affect three phase-localised regions of the pulse profile that exhibit coupled and anti-correlated temporal evolution. We also identified, and corrected for, systematic profile variability induced by polarization calibration errors arising from long-term drift of the polarimetric properties of the receiver. The profile change exhibits frequency-dependent evolution in total intensity, together with variations in linear polarization, position angle and fractional linear polarization. These results confirm a magnetospheric origin for the events rather than propagation effects caused by the interstellar medium, and provide potential new constraints on MSP emission models.
Comments18 pages, 10 figures, submitted to MNRAS
