Evidence for magnetospheric effects on the radiation of radio pulsars
Evidence for magnetospheric effects on the radiation of radio pulsars
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DOI：
10.1093/mnras/sty3315
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发表时间：
2018-11
影响因子：
4.8
通讯作者：
C. Ilie;S. Johnston;P. Weltevrede
中科院分区：
文献类型：
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作者：
C. Ilie;S. Johnston;P. Weltevrede
我们对射电脉冲星极化信号中相位分辨、明显RM变化的起源进行了迄今为止规模最大的调查。根据帕克斯射电望远镜在1.4 GHz波段观测到的98颗脉冲星样本，我们仔细量化了测量均方根的系统和统计误差。共有42颗脉冲星显示出明显的相位分辨RM变化。我们表明磁层效应和散射效应都能引起这些明显的变化。除了偏离法拉第定律外，复杂剖面与RM变异性程度之间存在明显的相关性。因此，我们得出结论，散射不能是RM变化的唯一原因，并给出了磁层效应占主导地位的清晰例子。只要有足够的信噪比，所有的射电脉冲星都可能出现这种效应。这些特征提供了一种工具来探测无线电发射在磁层中的传播。
We have conducted the largest investigation to date into the origin of phase resolved, apparent RM variations in the polarized signals of radio pulsars. From a sample of 98 pulsars based on observations at 1.4 GHz with the Parkes radio telescope, we carefully quantified systematic and statistical errors on the measured RMs. A total of 42 pulsars showed significant phase resolved RM variations. We show that both magnetospheric and scattering effects can cause these apparent variations. There is a clear correlation between complex profiles and the degree of RM variability, in addition to deviations from the Faraday law. Therefore, we conclude that scattering cannot be the only cause of RM variations, and show clear examples where magnetospheric effects dominate. It is likely that, given sufficient signal-to-noise, such effects will be present in all radio pulsars. These signatures provide a tool to probe the propagation of the radio emission through the magnetosphere.